Astronomy c ESO 2009 Astrophysics - UHRA Home
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A&A 505, 441–462 (2009) DOI: 10.1051/0004-6361/200912531 c ESO 2009 Astronomy & Astrophysics High-resolution UVES/VLT spectra of white dwarfs observed for the ESO SN Ia Progenitor Survey III. DA white dwarfs D. Koester 1 , B. Voss 2,1 , R. Napiwotzki 3 , N. Christlieb 4 , D. Homeier 5 , T. Lisker 6,8 , D. Reimers 7 , and U. Heber 8 1 Institut für Theoretische Physik und Astrophysik, Universität Kiel, 24098 Kiel, Germany e-mail: [email protected] 2 Zeiss-Planetarium, LWL-Museum für Naturkunde, 48161 Münster, Germany 3 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK 4 Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany 5 Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany 6 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12–14, 69120 Heidelberg, Germany 7 Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany 8 Dr. Karl Remeis Observatory, University of Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, Germany Received 19 May 2009 / Accepted 24 July 2009 ABSTRACT Context. The ESO Supernova Ia Progenitor Survey (SPY) took high-resolution spectra of more than 1000 white dwarfs and pre-white dwarfs. About two thirds of the stars observed are hydrogen-dominated DA white dwarfs. Here we present a catalog and detailed spectroscopic analysis of the DA stars in the SPY. Aims. Atmospheric parameters effective temperature and surface gravity are determined for normal DAs. Double-degenerate binaries, DAs with magnetic fields or dM companions, are classified and discussed. Methods. The spectra are compared with theoretical model atmospheres using a χ 2 fitting technique. Results. Our final sample contains 615 DAs, which show only hydrogen features in their spectra, although some are double-degenerate binaries. 187 are new detections or classifications. We also find 10 magnetic DAs (4 new) and 46 DA+dM pairs (10 new). Key words. stars: white dwarfs 1. Introduction The ESO SN Ia Progenitor Survey (SPY) is a radial velocity sur- vey that was conducted to test the double-degenerate channel of the formation of supernovae Ia. About 800 white dwarfs were observed (most of them twice) in the course of the survey, as- sembling a large collection of high quality white dwarf spectra. Most of the targets for the SPY were selected from the White Dwarf catalog (McCook & Sion 1999), MCS further on, from the Hamburg/ESO Survey (Wisotzki et al. 1996; Christlieb et al. 2001), HES further on, and from the Hamburg Quasar Survey (Hagen et al. 1995), HQS further on. Some additional objects come from the Montreal-Cambridge survey (Demers et al. 1990; Lamontagne et al. 2000) and from the Edinburgh-Cape survey (Kilkenny et al. 1991). A detailed discussion of the target se- lection is given in Napiwotzki et al. (2001, 2003). While some of the input catalogs, e.g. HES and HQS, have fairly well un- derstood selection criteria, for the combined input catalog this would be very difficult, since the only criteria used were “spec- troscopic identification (at least from objective prism spectra) and B < 16.5” (Napiwotzki et al. 2001). The high quality spectra of white dwarfs were employed for a number of studies beyond the original scope of the SPY, Based on data obtained at the Paranal Observatory of the European Southern Observatory for programmes 165.H-0588 and 167.D-0407. the search for double-degenerate binaries. Koester et al. (2001) derived temperatures and gravities from a preliminary sample of about 200 objects; 71 helium-rich stars of spectral type DB and DBA were studied in Voss et al. (2007), and approximately 60 objects with detected Ca ii resonance lines were discussed in Koester et al. (2005). Pauli et al. (2003, 2006) studied the 3D kinematics using the SPY data, new DO and PG1159 stars have been identified by Werner et al. (2004). The hot subdwarf population has been studied by Lisker et al. (2005) and Stroeer et al. (2007). The number of newly detected white dwarfs is of course dwarfed by the results from the Sloan Digital Sky Survey (e.g. Kleinman et al. 2004; Eisenstein et al. 2006). It is also possible to extract samples with much better controlled and understood selection effects from the SDSS data base. Thus, we will not produce yet another white dwarf mass distribution or luminos- ity function here. However, our sample contains much brighter objects than the typical SDSS white dwarf. These objects, and in particular the magnetic stars, binaries, or new variables will be much easier to study in follow-up observations than the faint SDSS objects. Moreover, the white dwarf parameters presented here are an important ingredient of the kinematic studies men- tioned above and the analysis and interpretation of the binary results, starting with the simple distinction between helium core and carbon/oxygen core white dwarfs. Article published by EDP Sciences
Transcript of Astronomy c ESO 2009 Astrophysics - UHRA Home
A&A 505, 441–462 (2009)DOI: 10.1051/0004-6361/200912531c© ESO 2009
Astronomy&
Astrophysics
High-resolution UVES/VLT spectra of white dwarfsobserved for the ESO SN Ia Progenitor Survey
III. DA white dwarfs�
D. Koester1, B. Voss2,1, R. Napiwotzki3, N. Christlieb4, D. Homeier5, T. Lisker6,8, D. Reimers7, and U. Heber8
1 Institut für Theoretische Physik und Astrophysik, Universität Kiel, 24098 Kiel, Germanye-mail: [email protected]
2 Zeiss-Planetarium, LWL-Museum für Naturkunde, 48161 Münster, Germany3 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK4 Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany5 Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany6 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12–14, 69120 Heidelberg,
Germany7 Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany8 Dr. Karl Remeis Observatory, University of Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, Germany
Received 19 May 2009 / Accepted 24 July 2009
ABSTRACT
Context. The ESO Supernova Ia Progenitor Survey (SPY) took high-resolution spectra of more than 1000 white dwarfs and pre-whitedwarfs. About two thirds of the stars observed are hydrogen-dominated DA white dwarfs. Here we present a catalog and detailedspectroscopic analysis of the DA stars in the SPY.Aims. Atmospheric parameters effective temperature and surface gravity are determined for normal DAs. Double-degenerate binaries,DAs with magnetic fields or dM companions, are classified and discussed.Methods. The spectra are compared with theoretical model atmospheres using a χ2 fitting technique.Results. Our final sample contains 615 DAs, which show only hydrogen features in their spectra, although some are double-degeneratebinaries. 187 are new detections or classifications. We also find 10 magnetic DAs (4 new) and 46 DA+dM pairs (10 new).
Key words. stars: white dwarfs
1. Introduction
The ESO SN Ia Progenitor Survey (SPY) is a radial velocity sur-vey that was conducted to test the double-degenerate channel ofthe formation of supernovae Ia. About 800 white dwarfs wereobserved (most of them twice) in the course of the survey, as-sembling a large collection of high quality white dwarf spectra.Most of the targets for the SPY were selected from the WhiteDwarf catalog (McCook & Sion 1999), MCS further on, fromthe Hamburg/ESO Survey (Wisotzki et al. 1996; Christlieb et al.2001), HES further on, and from the Hamburg Quasar Survey(Hagen et al. 1995), HQS further on. Some additional objectscome from the Montreal-Cambridge survey (Demers et al. 1990;Lamontagne et al. 2000) and from the Edinburgh-Cape survey(Kilkenny et al. 1991). A detailed discussion of the target se-lection is given in Napiwotzki et al. (2001, 2003). While someof the input catalogs, e.g. HES and HQS, have fairly well un-derstood selection criteria, for the combined input catalog thiswould be very difficult, since the only criteria used were “spec-troscopic identification (at least from objective prism spectra)and B < 16.5” (Napiwotzki et al. 2001).
The high quality spectra of white dwarfs were employedfor a number of studies beyond the original scope of the SPY,
� Based on data obtained at the Paranal Observatory of the EuropeanSouthern Observatory for programmes 165.H-0588 and 167.D-0407.
the search for double-degenerate binaries. Koester et al. (2001)derived temperatures and gravities from a preliminary sampleof about 200 objects; 71 helium-rich stars of spectral type DBand DBA were studied in Voss et al. (2007), and approximately60 objects with detected Ca ii resonance lines were discussedin Koester et al. (2005). Pauli et al. (2003, 2006) studied the3D kinematics using the SPY data, new DO and PG1159 starshave been identified by Werner et al. (2004). The hot subdwarfpopulation has been studied by Lisker et al. (2005) and Stroeeret al. (2007).
The number of newly detected white dwarfs is of coursedwarfed by the results from the Sloan Digital Sky Survey (e.g.Kleinman et al. 2004; Eisenstein et al. 2006). It is also possibleto extract samples with much better controlled and understoodselection effects from the SDSS data base. Thus, we will notproduce yet another white dwarf mass distribution or luminos-ity function here. However, our sample contains much brighterobjects than the typical SDSS white dwarf. These objects, andin particular the magnetic stars, binaries, or new variables willbe much easier to study in follow-up observations than the faintSDSS objects. Moreover, the white dwarf parameters presentedhere are an important ingredient of the kinematic studies men-tioned above and the analysis and interpretation of the binaryresults, starting with the simple distinction between helium coreand carbon/oxygen core white dwarfs.
Article published by EDP Sciences
442 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs
2. Observations
Since several of the papers above have given a detailed descrip-tion of the data properties and further references, we only brieflysummarize this information here.
The spectra were obtained with UVES, a high resolutionechelle spectrograph at the ESO VLT telescope. UVES was usedin a dichroic mode, resulting in small gaps, ≈80 Å wide, at4580 Å and 5640 Å in the final merged spectrum. The spectralresolution at Hα is R = 18 500 or better, and the S/N per binnedpixel (0.05 Å) is S/N = 15 or higher. The total wavelength rangecovered is ≈3500 to 6650 Å.
The spectra were reduced with the ESO pipeline for UVES,including the merging of the echelle orders and the wavelengthcalibration. Koester et al. (2001) found that the quality of theseautomatically extracted spectra was very good, except for aquasi-periodic wave-like pattern that occurs in some of the spec-tra. The reduction has since been further improved by addi-tional processing by collaborators of the SPY at the Universityof Erlangen-Nürnberg.The most important step was utilizing thefeatureless spectra of DC white dwarfs to remove almost com-pletely the large scale variations of the spectral response func-tion (Napiwotzki et al. 2001, 2003). Some artifacts remain in thedata, but they do not significantly affect the spectral analysis.
2.1. Model atmosphere fits
The spectral analysis of these data was originally performedby Voss (2006). Since then, the models were significantly im-proved by including in a consistent way the Balmer line broad-ening due to simultaneous interactions with neutral and chargedperturbers. An up-to-date description of the methods and inputphysics is presented in Koester (2009). We have therefore re-peated the whole fitting process for all objects; the major differ-ences to Voss (2006) appear, as expected, at the cool end of theDA sequence.
The χ2 minimization fitting routine is based on theLevenberg-Marquardt algorithm (Press et al. 1992) to derive thebest fitting effective temperature and surface gravity for eachspectrum. Some more details on the fitting process can be foundin Homeier et al. (1998). For the present study we appliedpure hydrogen models and fitted the Balmer lines Hα to H9.To demonstrate the typical quality of the data and of the modelfits, we present the results for the arbitrarily chosen entries 301to 310 from Table 1. The header of each panel gives the name,effective temperature, and surface gravity of the fit. Shown arethe six lowest Balmer lines.
3. Data and atmospheric parameters for DAs
Table 1 lists the results of the model fitting for 615 apparentlynormal DA white dwarfs. Of those, 187 are newly identifiedDAs, 111 from the HES (Christlieb et al. 2001, designationHE) and 76 from the HQS (Homeier et al. 1998, designationHS) surveys. The primary designation of the objects in thefirst column is WD, if the objects appear in the SIMBAD orMCS databases and were known to be spectroscopically iden-tified white dwarfs prior to the start of the SPY. A few objectshave EC or MCT designations, if they were identified in theEdinburgh-Cape (Kilkenny et al. 1991) or Montreal-Cambridge-Tololo (Demers et al. 1990; Lamontagne et al. 2000) surveys,but don’t seem to have WD designations. Column 5 gives a fewalternative names. This list is not intended to be complete, butadditional information can easily be found in SIMBAD or MCS.
For the remainder of the objects we use HE or HS designa-tions, depending on the original catalog. In this case there arethree different meanings of Col. 5
– if empty, there is no entry in either the SIMBAD or theMCS database and we assume that this is a new detectionof the HQS or HES;
– if there is an entry in parentheses, this means that there isan entry in SIMBAD, but no spectroscopic identification asa white dwarf, at least not prior to identification in a publi-cation related to HQS, HES, or SPY. This mostly concernscatalogs of blue or large proper motion objects. Some objectsare also contained in more recent catalogs, e.g. Sloan DigitalSky Survey = SDSS (Adelman-McCarthy et al. 2008), orTwo Micron All Sky Survey = 2MASS, (Cutri et al. 2003),but not identified as white dwarfs;
– if there is a regular entry in Col. 5, this describes a re-cent spectroscopic identification, which was unknown at thetime of our target selection. Catalog entries here are SDSS(Kleinman et al. 2004; Eisenstein et al. 2006), BGK (Brownet al. 2006), Kawka06 (Kawka & Vennes 2006).
The magnitude column lists the V magnitude, if available fromthe SIMBAD or MCS databases. If the number is followed bya B, this is either a Johnson B magnitude, or, in most cases, aphotographic magnitude from the MCT, HQS, or HES surveys.mc denotes a Greenstein multichannel magnitude, obtained fromthe MCS catalog. The errors of the photographic magnitudes aretypically much larger (0.1−0.2 mag) than suggested by the twodecimal places, which are kept only to obtain a more homoge-neous table.
Since most stars have more than one spectrum observed, theparameters are the weighted averages of the individual solutions,with the inverse square of the formal 1σ uncertainties as weights.The 1σ final uncertainties given in Table 1 are obtained from theindividual values and should only be used as an indicator of thequality of the data. As is well known, with spectra of the qual-ity used here, the systematic errors from the reduction and fit-ting process are usually much larger than the purely statisticaluncertainties. We estimated more realistic uncertainties by com-paring the differences between solutions from several spectra ofthe same object. For 592 objects with multiple solutions we ob-tain standard deviations of σ(Teff) ≈ 2.5% and σ(log g) ≈ 0.09.These should be regarded as lower limits, because the differentspectra still used the same observational setup, theoretical mod-els, and fitting procedures. The uncertainties are definitely largerthan this at the high temperature end above 50 000 K, becauseNLTE effects are not considered in our models. They are alsolarger, in particular for the surface gravity, at temperatures be-low 8000 K, because the spectra become less sensitive to this pa-rameter, and because the neutral broadening of the Balmer lineshigher than Hγ is only approximative.
Another method to estimate the size of the uncertainties isthe comparison of results by different authors for the same ob-jects. The most interesting recent study is the work by Liebertet al. (2005) on the DA white dwarfs in the Palomar GreenSurvey. Eliminating DAs with Teff below 8000 K or above50 000 K (see above), as well as the double degenerates, leaves85 objects in common. Figure 2 shows the comparison for theeffective temperatures, and Fig. 3 for the surface gravities. Thesystematic shift in Teff for the whole sample is 1.2%, with ourtemperatures being slightly higher. For log g the shift is 0.08,with our values lower. We can estimate the intrinsic uncer-tainties of our determinations by first correcting for these sys-tematic shifts. Comparing the corrected parameters with those
D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs 443Ta
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444 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs
Tabl
e1.
cont
inue
d.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
MC
T01
10−1
617
01:1
3:14
.12−1
6:01
:45.
616
.37
B34
621
757.
747
0.01
52
MC
T01
11−3
806
01:1
4:03
.23−3
7:50
:41.
915
.48
B71
306
535
7.19
00.
024
2W
D01
12−1
9501
:15:
05.6
2−1
9:15
:20.
016
.20
BM
CT
0112−1
931
3636
418
77.
658
0.02
82
WD
0114−6
0501
:16:
19.5
5−6
0:16
:07.
614
.90
BH
K22
953−
1824
692
467.
754
0.00
62
WD
0114−0
3401
:16:
58.8
0−0
3:10
:55.
716
.20
BG
D82
1,G
R51
519
460
997.
771
0.01
92
WD
0124−2
5701
:26:
55.9
0−2
5:30
:53.
715
.66
BM
CT
0124−2
546,
GD
1352
2304
267
7.78
90.
010
2W
D01
26+
101
01:2
9:24
.38+
10:2
2:59
.714
.38
G00
2−04
0,W
OL
F72
8557
57.
621
0.01
02
WD
0127−0
5001
:30:
23.0
6−0
4:47
:57.
813
.60
HE
0127−0
503,
G27
1−08
116
718
237.
784
0.00
52
WD
0129−2
0501
:31:
39.2
1−2
0:19
:59.
114
.64
BM
CT
0129−2
035
1995
046
7.88
50.
008
2H
S01
29+
1041
01:3
1:45
.54+
10:5
6:59
.115
.60
B(N
LTT
5061
)16
738
447.
916
0.00
92
HS
0130+
0156
01:3
2:57
.38+
02:1
1:32
.616
.00
B(P
HL
1026
)41
083
155
7.74
20.
016
2H
E01
30−2
721
01:3
3:09
.08−2
7:05
:45.
016
.08
B(G
D13
72,K
UV
0130
8−27
21)
2188
045
7.90
20.
007
2H
E01
31+
0149
01:3
4:28
.46+
02:0
4:21
.414
.69
B(P
HL
1040
)15
228
347.
745
0.00
72
DD
sW
D01
33−1
1601
:36:
13.3
9−1
1:20
:31.
314
.10
G27
1−10
6,Z
ZC
ET
I12
249
157.
856
0.00
52
DA
VW
D01
35−0
5201
:37:
59.4
0−0
4:59
:44.
912
.84
G27
1−11
5,L
HS
1270
6942
107.
081
0.01
02
DD
dM
CT
0136−2
010
01:3
8:31
.67−1
9:54
:50.
616
.49
BP
HL
3537
8416
108.
405
0.01
22
DD
sM
CT
0138−4
014
01:4
0:10
.98−3
9:59
:24.
616
.37
BH
E01
38−4
014
2169
844
7.89
80.
007
2W
D01
37−2
9101
:40:
16.7
9−2
8:52
:53.
716
.04
BM
CT
0137−2
908,
GD
1384
2155
055
7.75
50.
009
2W
D01
38−2
3601
:40:
28.1
5−2
3:21
:22.
816
.10
BM
CT
0138−2
336,
PH
L11
0036
897
297
7.62
70.
039
2W
D01
40−3
9201
:42:
50.9
9−3
8:59
:06.
914
.37
MC
T01
40−3
914,
SB
702
2181
124
7.91
80.
004
2W
D01
43+
216
01:4
6:41
.34+
21:5
4:48
.115
.05
G94−9
,WO
LF
8292
229
8.34
00.
009
2W
D01
45−2
2101
:47:
21.7
6−2
1:56
:51.
415
.30
MC
T01
45−2
211,
GD
1400
1174
720
8.06
60.
007
2D
AV
WD
0145−2
5701
:48:
08.1
8−2
5:32
:44.
114
.51
2591
537
7.85
80.
005
2H
S01
45+
1737
01:4
8:21
.51+
17:5
2:13
.515
.70
B18
125
297.
894
0.00
62
HE
0145−0
610
01:4
8:22
.27−0
5:55
:36.
516
.45
B(P
HL
1166
,BP
SC
S22
962−
0027
)86
1310
8.01
70.
013
3H
E01
50+
0045
01:5
2:59
.22+
01:0
0:20
.216
.40
BS
DS
S12
625
957.
705
0.02
61
NO
V(3
)W
D01
51+
017
01:5
4:13
.88+
02:0
1:23
.515
.00
G07
3−00
4,G
159−
012
1244
025
7.83
60.
008
2N
OV
(2)
HE
0152−5
009
01:5
4:35
.98−4
9:55
:01.
916
.32
B(C
SI−
50−0
1527
,JL
265)
1318
543
7.65
10.
008
2W
D01
55+
069
01:5
7:41
.33+
07:1
2:03
.815
.34
GD
20,F
EIG
E17
2200
756
7.66
80.
008
2W
D01
58−2
2702
:00:
53.4
1−2
2:27
:35.
716
.00
BH
E01
58−2
24,P
HL
1251
6708
167
67.
463
0.03
12
HE
0201−0
513
02:0
3:37
.60−0
4:59
:12.
815
.94
B(P
B90
09,G
159−
31)
2462
610
27.
638
0.01
31
HS
0200+
2449
02:0
3:45
.80+
25:0
4:09
.115
.60
B23
281
537.
860
0.00
72
WD
0203−1
3802
:05:
49.0
5−1
3:38
:27.
415
.70
B48
529
275
7.99
70.
020
2W
D02
04−2
3302
:06:
45.1
0−2
3:16
:14.
015
.60
G27
4−15
0,L
P82
9−01
713
095
787.
775
0.01
02
HE
0204−3
821
02:0
6:47
.55−3
8:07
:04.
015
.60
B14
038
447.
794
0.00
62
HE
0204−4
213
02:0
6:49
.89−4
1:59
:25.
816
.43
B22
575
587.
902
0.00
92
WD
0205−3
6502
:07:
25.4
6−3
6:20
:49.
416
.10
BM
CT
0205−3
635
6124
044
87.
742
0.02
42
WD
0205−3
0402
:07:
40.8
6−3
0:10
:59.
615
.67
BG
D14
4217
209
317.
761
0.00
62
HE
0205−2
945
02:0
8:08
.00−2
9:31
:38.
816
.06
B10
476
107.
774
0.00
82
DD
dW
D02
08−2
6302
:10:
58.6
3−2
6:07
:01.
315
.80
BH
E02
08−2
621
3372
065
7.76
40.
012
2H
E02
10−2
012
02:1
3:01
.93−1
9:58
:35.
216
.29
B17
612
277.
800
0.00
62
HE
0211−2
824
02:1
3:56
.66−2
8:10
:17.
815
.27
B14
469
487.
951
0.00
32
WD
0212−2
3102
:14:
21.2
6−2
2:54
:49.
116
.40
BH
E02
12−2
308,
GR
286
2682
761
7.94
30.
009
2
D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs 445Ta
ble
1.co
ntin
ued.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
HS
0213+
1145
02:1
6:07
.61+
11:5
9:18
.915
.50
B17
518
847.
787
0.01
81
NO
VW
D02
16+
143
02:1
8:48
.27+
14:3
6:03
.214
.58
PG
0216+
144
2663
729
7.79
10.
005
2D
Ds
HE
0219−4
049
02:2
1:19
.69−4
0:35
:29.
716
.20
B15
373
367.
893
0.00
52
HE
0221−2
642
02:2
3:29
.40−2
6:29
:19.
715
.63
B32
008
447.
721
0.01
12
WD
0220+
222
02:2
3:36
.07+
22:2
7:28
.415
.83
G94−B
5B,E
G18
1563
065
7.89
00.
010
1H
E02
21−0
535
02:2
3:59
.88−0
5:21
:45.
915
.59
B(P
HL
1276
)24
747
497.
954
0.00
72
HE
0222−2
336
02:2
4:19
.89−2
3:23
:15.
616
.48
B31
816
817.
874
0.01
81
HE
0222−2
630
02:2
4:36
.06−2
6:16
:52.
215
.59
B23
198
387.
911
0.00
52
HS
0223+
1211
02:2
6:29
.98+
12:2
5:22
.816
.00
B14
721
867.
300
0.01
91
HE
0225−1
912
02:2
7:41
.43−1
8:59
:24.
516
.14
B(P
HL
1295
)17
269
377.
559
0.00
81
DD
dH
S02
25+
0010
02:2
7:55
.50+
00:2
3:39
.115
.90
B13
337
807.
835
0.01
02
WD
0226−3
2902
:28:
27.7
0−3
2:42
:35.
913
.73
BH
E02
26−3
255
2229
422
7.87
50.
003
3W
D02
27+
050
02:3
0:16
.66+
05:1
5:50
.712
.65
Fei
ge22
,EG
1919
341
127.
762
0.00
22
WD
0229−4
8102
:30:
53.3
1−4
7:55
:25.
914
.53
LB
1628
,RE
0230−4
7559
082
364
7.71
30.
020
2W
D02
31−0
5402
:34:
07.7
3−0
5:11
:39.
614
.24
GD
31,P
HL
1358
1730
611
8.44
50.
003
3H
S02
37+
1034
02:4
0:35
.57+
10:4
7:01
.516
.00
B17
259
707.
857
0.01
51
DD
sH
S02
41+
1411
02:4
4:00
.75+
14:2
4:29
.616
.20
B13
753
150
7.76
30.
019
1W
D02
42−1
7402
:45:
02.3
5−1
7:12
:20.
615
.33
HK
2218
9−19
2066
338
7.85
30.
007
1W
D02
43+
155
02:4
6:24
.06+
15:4
5:01
.916
.46
mc
PG
0243+
155
1761
161
7.95
80.
013
1H
E02
45−0
008
02:4
7:46
.45+
00:0
3:30
.416
.45
BS
DS
S18
813
115
7.97
70.
022
1H
E02
46−5
449
02:4
8:07
.16−5
4:36
:44.
916
.39
B15
949
457.
829
0.01
02
WD
0250−0
2602
:52:
51.0
5−0
2:25
:17.
414
.73
HE
0250−0
237,
KU
V02
503−
0238
1531
523
7.79
70.
005
2W
D02
50−0
0702
:53:
32.2
9−0
0:33
:45.
316
.40
KU
V02
510-
0046
,SD
SS
7948
137.
793
0.01
92
WD
0252−3
5002
:54:
37.2
5−3
4:49
:56.
615
.89
BH
E02
52−3
501
1693
434
7.36
60.
007
2W
D02
55−7
0502
:56:
16.9
0−7
0:22
:17.
714
.08
L54−5
,LF
T24
510
514
88.
080
0.00
62
NO
V(1
)H
E02
55−1
100
02:5
8:21
.72−1
0:48
:25.
715
.99
B(P
B94
04)
2082
713
27.
836
0.02
01
HE
0256−1
802
02:5
8:59
.54−1
7:50
:20.
316
.41
B26
212
627.
757
0.01
02
HE
0257−2
104
02:5
9:52
.65−2
0:52
:49.
616
.30
B17
362
427.
692
0.00
82
HE
0300−2
313
03:0
2:36
.69−2
3:01
:52.
015
.35
B22
369
378.
386
0.00
52
WD
0302+
027
03:0
4:37
.40+
02:5
6:56
.614
.97
GD
41,F
EIG
E31
3527
061
7.77
20.
009
2H
E03
03−2
041
03:0
6:04
.96−2
0:29
:31.
116
.26
B(P
HL
1467
)10
006
108.
131
0.01
02
HE
0305−1
145
03:0
8:10
.25−1
1:33
:45.
715
.40
B(P
HL
8567
)26
822
687.
812
0.01
02
WD
0307+
149
03:0
9:53
.95+
15:0
5:22
.115
.10
BH
S03
7+14
54,P
G03
07+
149
2141
327
7.90
90.
004
2H
S03
07+
0746
03:1
0:09
.13+
07:5
7:32
.616
.50
B10
127
148.
070
0.01
32
WD
0310−6
8803
:10:
30.9
9−6
8:36
:03.
311
.40
CP
D−6
9◦17
7,L
B33
0316
329
67.
908
0.00
14
HE
0308−2
305
03:1
1:07
.24−2
2:54
:05.
615
.16
B23
565
418.
538
0.00
62
WD
0308+
188
03:1
1:49
.22+
19:0
0:55
.513
.86
BP
G03
08+
188
1845
021
7.72
50.
004
2H
S03
09+
1001
03:1
2:34
.96+
10:1
2:27
.215
.60
B18
786
317.
725
0.00
62
WD
0315−3
3203
:17:
26.0
5−3
3:03
:05.
416
.53
BH
E03
15−3
314
4992
635
07.
472
0.02
53
HS
0315+
0858
03:1
7:43
.18+
09:0
9:55
.215
.90
B18
783
387.
871
0.00
72
HE
0315−0
118
03:1
8:13
.31−0
1:07
:13.
114
.71
BS
DS
S13
469
517.
614
0.00
72
DD
dH
E03
17−2
120
03:1
9:27
.22−2
1:09
:13.
215
.80
B96
8813
8.09
30.
014
2W
D03
17+
196
03:2
0:04
.07+
19:4
7:35
.415
.58
BP
G03
17+
196
1773
550
7.77
60.
011
1
446 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs
Tabl
e1.
cont
inue
d.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
WD
0318−0
2103
:20:
58.7
7−0
1:59
:59.
516
.01
HE
0318−0
210,
KU
V03
184−
0211
1512
545
7.70
20.
008
2W
D03
20−5
3903
:22:
14.8
1−5
3:45
:16.
314
.99
BL
B16
63,R
EJ0
322−
534
3258
828
7.76
90.
006
3H
E03
20−1
917
03:2
2:31
.91−1
9:06
:47.
816
.00
B(P
HL
4402
)13
248
887.
168
0.01
62
DD
sH
E03
24−2
234
03:2
6:26
.88−2
2:24
:15.
016
.39
B(P
HL
1537
)16
905
357.
845
0.00
82
HE
0324−0
646
03:2
6:39
.97−0
6:36
:05.
215
.95
BB
GK
,SD
SS
1574
041
7.86
60.
008
2H
E03
24−1
942
03:2
7:05
.02−1
9:32
:23.
816
.25
B(P
HL
1541
)20
660
498.
078
0.00
82
DD
dH
E03
25−4
033
03:2
7:43
.92−4
0:23
:26.
116
.38
B16
737
507.
695
0.01
02
DD
sH
S03
25+
2142
03:2
8:25
.24+
21:5
3:08
.415
.30
B13
863
118
7.93
50.
011
1W
D03
26−2
7303
:28:
48.8
1−2
7:19
:01.
714
.00
LP
888−
064,
L05
87−0
77A
9190
57.
717
0.00
62
DD
sW
D03
28+
008
03:3
1:33
.93+
01:0
3:26
.516
.80
HE
0328+
0053
,SD
SS
3447
611
37.
920
0.02
22
HE
0330−4
736
03:3
2:03
.98−4
7:25
:57.
716
.03
B12
913
388.
034
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HS
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1121
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2:35
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11:3
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855
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81
WD
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36.9
0−0
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615
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0100
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459
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00.
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783
0.00
91
HE
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6:02
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515
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HE
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616
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WD
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25.2
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82
HS
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08:0
4:53
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796
707.
720
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42
WD
0346−0
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50.2
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0:58
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213
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GD
50,G
R28
8,S
DS
S40
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313
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92
HE
0348−4
445
03:4
9:59
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4:36
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416
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951
398.
069
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72
HE
0348−2
404
03:5
0:38
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3:55
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216
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735
547.
944
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62
HE
0349−2
537
03:5
1:41
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5:28
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615
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974
447.
906
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82
WD
0352+
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4:40
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312
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V03
520+
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967
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42
WD
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018
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4:43
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8:41
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HE
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V03
521+
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758
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70.
008
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52+
096
03:5
5:22
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7:17
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HS
0352+
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414
440
478.
178
0.00
52
HE
0358−5
127
03:5
9:38
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1:18
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515
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376
477.
927
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62
HS
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1451
04:0
3:42
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9:28
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618.
250
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52
HS
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1454
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2:26
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11
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702
627.
937
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7:11
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516
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1
D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs 447Ta
ble
1.co
ntin
ued.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
WD
0406+
169
04:0
9:28
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17:0
7:54
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7−11
2,L
P41
4−10
116
049
488.
236
0.00
81
WD
0407+
179
04:1
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18:0
2:24
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1754
1442
12
7.76
80.
003
3N
OV
(1)
WD
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02.1
7−0
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215
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115
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457.
856
0.01
01
HE
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154
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1:46
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815
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315
677.
830
0.00
92
HE
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2:28
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316
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347.
601
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72
DD
dW
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HS
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1144
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42
HS
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812
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HE
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935
0.01
02
WD
0416−5
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11.5
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16−5
505
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80.
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8:45
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616
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324
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846
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168
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916
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386
217.
854
0.00
42
WD
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106
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8:58
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826
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4:48
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129
557.
989
0.00
52
WD
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968
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52
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633
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6:27
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959
0.00
62
WD
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152
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139
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3804
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07.0
7−0
3:46
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516
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861
88.
420
0.02
72
WD
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46.6
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8:51
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213
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BP
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627
227.
687
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32
HE
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429
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916
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825
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810
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81
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444
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407.
839
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72
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315
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553
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33
DD
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682
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92
HS
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0154
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544
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8:51
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316
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421
488.
271
0.00
82
HS
0507+
0434
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13.5
9+
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8:54
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818
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14.0
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2083
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70.
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2H
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738
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WD
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06.5
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213
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RE
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127.
228
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52
WD
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23.0
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1:45
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680
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42
HE
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1W
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18.9
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DA
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71,L
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167.
731
0.00
33
448 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfsTa
ble
1.co
ntin
ued.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
WD
0556+
172
05:5
9:44
.95+
17:1
2:03
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KP
D05
56+
1712
1882
531
8.09
40.
006
2W
D05
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165
06:0
1:17
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16:3
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KP
D05
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1631
1680
727
8.18
30.
005
2W
D06
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8306
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02.7
5−4
8:19
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816
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3473
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7.84
20.
012
2W
D06
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177
06:1
5:18
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17:4
3:40
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2562
424
7.81
40.
003
2W
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7606
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12.7
1−3
7:41
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812
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RE
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74,E
UV
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623−
376
5780
612
07.
269
0.00
62
WD
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2006
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38.5
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2:05
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015
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P60
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127.
248
0.02
31
WD
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5006
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57.7
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5:05
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815
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RE
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50,E
UV
EJ0
632−
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335
0.01
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WD
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8:32
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56.2
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213
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10.
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55.0
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0:25
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514
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674
0.01
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WD
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40.
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D07
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37.8
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31.9
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2:59
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RE
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50.
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24:5
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660
0.01
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WD
0830−5
3508
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52.0
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3:40
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763
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WD
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SS
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192
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5:30
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15:5
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HS
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1603
1606
434
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40.
008
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3909
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17.3
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4:06
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312
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114
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20.
002
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007
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22.3
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7:51
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616
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0911
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175
347.
854
0.00
72
WD
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064
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06:1
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BP
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SD
SS
4304
823
27.
368
0.02
11
WD
0922+
162B
09:2
5:13
.22+
16:0
1:45
.617
.30
2578
317
89.
039
0.02
81
WD
0922+
162A
09:2
5:13
.55+
16:0
1:44
.716
.26
2353
748
8.22
60.
008
3W
D09
22+
183
09:2
5:18
.37+
18:0
5:34
.316
.46
mc
PG
0922+
183
2453
259
8.15
90.
008
2W
D09
28−7
1309
:29:
08.6
5−7
1:34
:02.
815
.44
L64−4
0,B
PM
0563
983
896
8.05
70.
009
3H
S09
26+
0828
09:2
9:36
.53+
08:1
5:46
.816
.20
B(S
DS
S)
1493
965
7.70
00.
013
2N
OV
(3)
1202
751
7.91
10.
015
2am
bH
S09
29+
0839
09:3
2:29
.85+
08:2
6:37
.516
.10
BB
GK
1570
739
7.77
40.
014
2H
S09
31+
0712
09:3
4:32
.67+
06:5
8:48
.216
.50
BS
DS
S36
719
193
7.16
00.
025
2H
S09
33+
0028
09:3
6:07
.96+
00:1
4:35
.916
.00
B32
219
698.
100
0.01
62
HS
0937+
0130
09:3
9:58
.67+
01:1
6:38
.216
.50
BS
DS
S19
717
478.
314
0.00
82
WD
0937−1
0309
:40:
11.9
6−1
0:34
:25.
115
.97
EC
0937
7−10
2017
562
308.
502
0.00
52
WD
0939−1
5309
:41:
56.2
2−1
5:32
:14.
615
.92
EC
0939
5−15
1813
500
587.
787
0.00
72
HS
0940+
1129
09:4
3:14
.38+
11:1
6:11
.416
.10
B15
176
497.
838
0.00
92
1303
112
87.
878
0.01
41
amb
HS
0943+
1401
09:4
6:31
.60+
13:4
7:35
.816
.40
B16
863
258.
275
0.01
02
HS
0944+
1913
09:4
7:31
.67+
18:5
9:12
.715
.30
B17
444
177.
883
0.00
32
HS
0949+
0935
09:5
1:48
.94+
09:2
1:12
.616
.30
B(S
DS
S)
1835
765
7.69
40.
013
2H
S09
49+
0823
09:5
1:56
.17+
08:0
9:33
.716
.10
B14
755
667.
808
0.01
22
NO
V(3
)W
D09
50+
077
09:5
2:59
.15+
07:3
1:08
.316
.12
BP
G09
50+
078
1562
337
7.89
10.
006
2
D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs 449
Tabl
e1.
cont
inue
d.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
WD
0951−1
5509
:53:
40.3
6−1
5:48
:56.
616
.09
EC
0951
2−15
3417
973
337.
827
0.00
72
WD
0954+
134
09:5
7:18
.99+
13:1
2:57
.016
.41
BP
G09
54+
135,
SD
SS
1646
275
7.67
70.
015
2W
D09
55+
247
09:5
7:48
.37+
24:3
2:55
.515
.07
G49−3
3,LT
T12
661
8446
67.
985
0.00
92
WD
0956+
045
09:5
8:37
.24+
04:2
1:31
.015
.80
mc
PG
0956+
046
1822
841
7.77
90.
008
3W
D09
56+
020
09:5
8:50
.49+
01:4
7:23
.515
.61
BH
E09
56+
0201
,PG
0956+
021,
SD
SS
1649
525
7.80
60.
006
2W
D10
00−0
0110
:03:
16.3
4−0
0:23
:36.
916
.08
mc
PG
1000−0
02,L
B56
420
253
507.
803
0.00
92
WD
1003−0
2310
:05:
51.5
4−0
2:34
:19.
515
.43
PG
1003−0
2320
614
357.
889
0.00
62
HS
1003+
0726
10:0
6:23
.08+
07:1
2:12
.615
.30
BS
DS
S94
8616
8.02
00.
018
1W
D10
10+
043
10:1
3:12
.78+
04:0
5:12
.816
.34
BP
G10
10+
043
2861
756
7.90
30.
010
2H
E10
12−0
049
10:1
5:11
.75−0
1:04
:17.
115
.57
B(2
MA
SS
)23
204
478.
074
0.00
72
HS
1013+
0321
10:1
5:48
.15+
03:0
6:46
.815
.60
BS
DS
S11
600
247.
983
0.01
02
DA
VW
D10
13−0
1010
:16:
07.0
1−0
1:19
:18.
715
.33
G05
3−03
8,E
G25
380
666
7.50
90.
011
2D
Ds
WD
1015−2
1610
:17:
26.6
7−2
1:53
:43.
415
.66
EC
1015
0−21
3830
937
407.
891
0.00
82
WD
1015+
076
10:1
8:01
.69+
07:2
1:22
.415
.37
PG
1015+
076
2737
512
47.
728
0.01
81
WD
1015+
161
10:1
8:03
.84+
15:5
1:58
.315
.57
mc
PG
1015+
161
1994
833
7.92
50.
006
2W
D10
17−1
3810
:19:
52.4
5−1
4:07
:35.
514
.56
EC
1017
4−13
52,R
EJ1
019−
140
3179
826
7.84
50.
006
2W
D10
17+
125
10:1
9:56
.02+
12:1
6:29
.915
.75
mc
PG
1017+
125
2138
643
7.87
50.
007
2W
D10
19+
129
10:2
2:28
.77+
12:4
1:59
.415
.60
PG
1019+
129
1841
229
7.88
50.
006
2W
D10
20−2
0710
:22:
43.8
3−2
1:00
:02.
115
.09
EC
1020
3−20
4419
920
587.
926
0.01
01
WD
1022+
050
10:2
4:59
.90+
04:4
6:09
.014
.18
PG
1022+
050,
LP
550−
5214
693
557.
364
0.01
21
DD
s,N
OV
(2)
WD
1023+
009
10:2
5:49
.77+
00:3
9:04
.416
.40
mc
PG
1023+
009
3781
715
77.
650
0.01
72
WD
1026+
023
10:2
9:09
.87+
02:0
5:49
.714
.20
mc
PG
1026+
024,
LP
550−
292
1233
818
7.95
50.
004
3N
OV
(2)
WD
1031−1
1410
:33:
42.7
9−1
1:41
:40.
413
.00
EC
1031
2−11
26,L
0825−0
1425
502
277.
845
0.00
41
WD
1031+
063
10:3
4:05
.43+
06:0
2:45
.616
.26
mc
PG
1031+
063
2131
767
7.75
90.
010
2W
D10
36+
085
10:3
9:07
.48+
08:1
8:39
.116
.07
BP
G10
36+
086
2292
493
7.32
40.
012
2H
S10
43+
0258
10:4
6:23
.34+
02:4
2:35
.615
.60
BS
DS
S13
739
747.
756
0.01
02
WD
1049−1
5810
:52:
20.6
9−1
6:08
:05.
914
.36
EC
1049
8−15
5220
037
238.
276
0.00
42
WD
1053−5
5010
:55:
13.7
7−5
5:19
:05.
814
.32
L25
0−52
,BP
M20
383
1462
120
7.85
70.
004
2N
OV
(1)
WD
1053−2
9010
:55:
40.0
4− 2
9:19
:53.
415
.38
EC
1053
2−29
0310
664
108.
068
0.00
62
WD
1053−0
9210
:55:
45.4
1−0
9:30
:59.
116
.38
BH
E10
53−0
914,
PG
1053−0
9222
620
617.
694
0.00
92
HS
1053+
0844
10:5
5:51
.54+
08:2
8:46
.616
.50
B16
556
497.
813
0.01
12
WD
1056−3
8410
:58:
20.1
9−3
8:44
:26.
514
.08
RE
1058−3
84,E
UV
EJ1
058−
387
2794
725
7.89
80.
004
2W
D10
58−1
2911
:01:
12.2
8−1
3:14
:42.
714
.93
EC
1058
7−12
58,P
G10
58−1
2923
892
328.
651
0.00
54
HS
1102+
0934
11:0
4:36
.76+
09:1
8:22
.716
.40
BB
GK
,SD
SS
1696
155
7.36
70.
012
3D
Ds
WD
1102−1
8311
:04:
47.0
8−1
8:37
:15.
215
.99
EC
1102
3−18
2180
578
7.85
10.
011
3H
S11
02+
0032
11:0
5:15
.33+
00:1
6:26
.314
.80
(SD
SS
,GD
127)
1261
049
8.24
20.
011
2N
OV
(3)
WD
1105−0
4811
:07:
59.9
8−0
5:09
:27.
312
.92
LP
672−
001,
G16
3−05
015
995
117.
753
0.00
22
HS
1115+
0321
11:1
7:46
.18+
03:0
4:51
.315
.40
BB
GK
,SD
SS
,GD
131
1426
739
7.70
90.
007
2W
D11
16+
026
11:1
9:12
.55+
02:2
0:30
.914
.57
GD
133,
PG
1116+
026
1212
123
8.00
50.
005
2D
AV
HE
1117−0
222
11:1
9:34
.66−0
2:39
:06.
314
.25
B(G
D13
5)14
709
367.
978
0.00
52
WD
1121+
216
11:2
4:13
.08+
21:2
1:34
.814
.23
G12
0−45
,LH
S30
469
297
7.30
60.
011
2W
D11
22−3
2411
:24:
35.6
2−3
2:46
:25.
715
.86
EC
1122
1−32
2921
671
387.
855
0.00
62
WD
1123+
189
11:2
6:19
.11+
18:3
9:17
.214
.01
mc
PG
1123+
189,
RE
J112
6+18
358
126
205
7.49
80.
012
2H
E11
24+
0144
11:2
6:49
.74+
01:2
7:56
.416
.30
BG
K,S
DS
S16
246
357.
743
0.00
72
WD
1124−2
9311
:27:
09.3
2−2
9:40
:11.
815
.02
EC
1124
6−29
23,E
SO
0439−0
8093
976
8.09
90.
007
2W
D11
24−0
1811
:27:
21.3
3−0
2:08
:37.
716
.47
mc
PG
1124−0
19,S
DS
S23
942
457.
628
0.00
92
DD
s
450 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfsTa
ble
1.co
ntin
ued.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
WD
1125−0
2511
:28:
14.5
0−0
2:50
:27.
315
.32
BP
G11
25−0
26,R
EJ1
128−
025
3175
536
8.15
90.
008
2W
D11
25+
175
11:2
8:15
.68+
17:1
4:06
.915
.95
PG
1125+
175
6121
348
47.
490
0.02
72
WD
1126−2
2211
:29:
11.6
4−2
2:33
:44.
416
.17
EC
1126
6−22
1711
818
418.
009
0.01
22
DA
VW
D11
29+
071
11:3
2:03
.58+
06:5
5:07
.914
.90
mc
PG
1129+
072
1459
935
7.83
10.
006
2W
D11
29+
155
11:3
2:27
.46+
15:1
7:29
.114
.04
mc
PG
1129+
156
1773
916
8.02
90.
003
2W
D11
30−1
2511
:33:
19.5
0−1
2:49
:01.
215
.50
EC
1130
7−12
3214
138
618.
342
0.00
82
HS
1136+
1359
11:3
9:25
.42+
13:4
3:11
.016
.00
B(A
111
7)23
921
204
7.82
80.
028
1H
S11
36+
0326
11:3
9:26
.64+
03:1
0:19
.716
.20
B13
530
126
7.92
60.
017
2W
D11
41+
077
11:4
3:59
.45+
07:2
9:04
.714
.11
BP
G11
41+
078
6249
334
57.
554
0.01
81
WD
1144−2
4611
:47:
20.1
3−2
4:54
:56.
715
.71
EC
1144
8−24
3830
500
417.
161
0.00
92
HS
1144+
1517
11:4
7:25
.13+
15:0
0:38
.716
.30
BB
GK
,SD
SS
1538
559
7.77
30.
013
2W
D11
45+
187
11:4
8:03
.18+
18:3
0:46
.614
.22
PG
1145+
188,
RE
J114
8+18
327
167
277.
798
0.00
42
WD
1147+
255
11:5
0:20
.18+
25:1
8:32
.615
.55
G12
1−02
2,H
S14
06+
2229
9910
118.
046
0.01
12
NO
V(1
)W
D11
49+
057
11:5
1:54
.29+
05:2
8:38
.314
.91
mc
PG
1149+
058,
SD
SS
1102
321
8.05
70.
012
3D
AV
WD
1150−1
5311
:53:
15.3
7−1
5:36
:36.
816
.00
EC
1150
7−15
1912
132
428.
033
0.00
82
DA
VH
E11
52−1
244
11:5
4:34
.91−1
3:01
:16.
815
.81
B13
126
547.
780
0.00
62
WD
1152−2
8711
:54:
45.8
2−2
9:00
:40.
716
.38
EC
1152
2−28
4320
620
797.
628
0.01
31
HS
1153+
1416
11:5
5:59
.76+
14:0
0:13
.315
.80
(PB
3724
)15
553
657.
785
0.01
42
WD
1155−2
4311
:57:
33.6
5−2
4:39
:27.
916
.48
EC
1155
0−24
2213
831
967.
888
0.01
12
WD
1159−0
9812
:02:
07.7
1−1
0:04
:40.
815
.97
mc
HE
1159−0
947,
LP
734−
006
9261
88.
537
0.00
82
WD
1201−0
0112
:03:
47.5
3−0
0:23
:11.
815
.12
mc
HE
1201−0
06,S
DS
S19
853
278.
295
0.00
52
WD
1202−2
3212
:05:
26.8
0−2
3:33
:13.
612
.79
EC
1202
8−23
1686
154
8.04
20.
006
2W
D12
04−3
2212
:06:
47.6
3−3
2:34
:33.
815
.68
EC
1204
2−32
17,H
E12
04−3
217
2126
341
7.99
60.
007
2W
D12
04−1
3612
:06:
56.4
3−1
3:53
:53.
615
.52
EC
1204
3−13
3710
939
168.
190
0.00
82
NO
V(4
)H
S12
04+
0159
12:0
7:29
.51+
01:4
2:50
.616
.50
B24
756
867.
755
0.01
12
WD
1207−1
5712
:10:
09.3
4−1
6:00
:40.
416
.32
EC
1207
5−15
43,H
E12
07−1
543
1688
548
7.77
50.
010
2W
D12
10+
140
12:1
2:33
.89+
13:4
6:25
.114
.67
3212
736
6.92
40.
008
2D
Ds
WD
1214+
032
12:1
6:51
.84+
02:5
8:04
.315
.32
LP
544−
063,
SD
SS
6272
146.
915
0.03
01
HE
1215+
0227
12:1
7:56
.20+
02:1
0:45
.816
.35
B(S
DS
S)
5969
172
37.
595
0.04
02
WD
1216+
036
12:1
8:41
.15+
03:2
0:21
.715
.94
mc
PG
1216+
036,
SD
SS
1440
43
7.76
90.
009
2W
D12
18−1
9812
:21:
07.3
5−2
0:07
:05.
116
.35
EC
1218
5−19
5035
013
817.
912
0.01
52
WD
1220−2
9212
:23:
05.1
7−2
9:32
:28.
915
.79
EC
1220
4−29
1517
702
297.
890
0.00
52
HE
1225+
0038
12:2
8:07
.72+
00:2
2:19
.615
.09
B(S
DS
S)
9383
58.
094
0.00
53
WD
1229−0
1212
:31:
34.4
6−0
1:32
:08.
514
.24
HE
1229−0
115,
SD
SS
1954
021
7.50
00.
004
2W
D12
30−3
0812
:33:
00.6
7−3
1:08
:36.
415
.81
EC
1230
3−30
5222
764
388.
280
0.00
62
WD
1231−1
4112
:33:
36.8
9−1
4:25
:08.
616
.12
EC
1231
0−14
0817
217
357.
923
0.00
72
WD
1233−1
6412
:36:
14.0
2−1
6:41
:53.
515
.10
EC
1233
6−16
2524
892
338.
207
0.00
43
WD
1236−4
9512
:38:
50.0
2−4
9:48
:01.
113
.96
L32
7−18
6,LT
T48
1611
372
128.
743
0.00
42
DA
VW
D12
37−0
2812
:40:
09.6
6−0
3:10
:14.
815
.97
mc
PG
1237−0
29,S
DS
S99
3613
8.42
10.
012
2W
D12
41+
235
12:4
4:16
.57+
23:1
4:10
.815
.18
mc
PG
1241+
235,
LB
1626
982
507.
772
0.00
82
WD
1241−0
1012
:44:
28.6
6−0
1:18
:59.
614
.00
PG
1241−0
10,S
DS
S23
459
257.
379
0.00
32
DD
dH
S12
43+
0132
12:4
5:38
.74+
01:1
6:16
.115
.60
B(U
M51
7,L
ED
A43
016)
2164
465
7.81
70.
010
2W
D12
44−1
2512
:47:
26.8
8−1
2:48
:42.
014
.70
EC
1244
8−12
3213
429
397.
928
0.00
52
HE
1247−1
130
12:4
9:54
.26−1
1:47
:00.
214
.74
B28
110
627.
840
0.01
12
EC
1248
9−27
5012
:51:
41.0
8−2
8:06
:48.
816
.22
6104
545
97.
628
0.02
32
HS
1249+
0426
12:5
2:15
.19+
04:1
0:43
.015
.80
B(P
B43
04)
1138
219
8.02
90.
009
2D
AV
WD
1249+
160
12:5
2:17
.15+
15:4
4:43
.414
.63
GD
150,
SD
SS
2579
240
7.21
40.
006
2
D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs 451Ta
ble
1.co
ntin
ued.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
WD
1249+
182
12:5
2:23
.34+
17:5
6:53
.915
.48
GD
151
1991
125
7.72
90.
004
2H
E12
52−0
202
12:5
4:58
.10−0
2:18
:36.
716
.50
B(B
GK
,SD
SS
)15
934
647.
806
0.01
52
WD
1254+
223
12:5
7:02
.33+
22:0
1:52
.713
.33
GD
153,
BP
M88
611,
SD
SS
3953
742
7.58
70.
005
2W
D12
57+
047
12:5
9:50
.35+
04:3
1:26
.614
.99
GD
267,
LP
556−
035,
SD
SS
2175
932
7.94
90.
005
2W
D12
57+
032
12:5
9:56
.69+
02:5
5:56
.215
.60
BP
G12
57+
032,
PB
4421
,SD
SS
1757
924
7.81
40.
005
2H
E12
58+
0123
13:0
1:10
.50+
01:0
7:39
.916
.42
B(S
DS
S,2
MA
SS
)11
258
227.
946
0.01
32
DA
VW
D13
00−0
9813
:03:
16.7
7−1
0:09
:12.
516
.25
BP
G13
00−0
9915
327
638.
143
0.00
82
NO
VH
S13
05+
0029
13:0
8:20
.87+
00:1
3:30
.516
.20
BB
GK
,SD
SS
1472
551
7.84
60.
008
2H
E13
07−0
059
13:0
9:41
.67−0
1:15
:05.
915
.72
B18
191
457.
907
0.00
92
HS
1308+
1646
13:1
1:06
.06+
16:3
1:03
.415
.50
B10
727
158.
242
0.01
12
NO
VW
D13
08−3
0113
:11:
17.5
2−3
0:25
:57.
615
.11
EC
1308
5−30
1014
422
337.
899
0.00
42
HE
1310−0
337
13:1
3:28
.35−0
3:53
:19.
716
.31
B18
943
737.
825
0.01
31
WD
1310−3
0513
:13:
41.5
9−3
0:51
:33.
714
.48
EC
1310
9−30
3520
353
227.
819
0.00
43
EC
1312
3−25
2313
:15:
03.9
4−2
5:39
:01.
015
.69
7546
382
57.
682
0.02
71
WD
1314−1
5313
:16:
43.5
9−1
5:35
:58.
714
.86
EC
1314
0−15
20,L
HS
2712
1615
225
7.72
00.
005
3W
D13
14−0
6713
:17:
18.4
6−0
6:59
:28.
115
.87
BP
G13
14−0
6716
832
527.
847
0.01
12
HE
1315−1
105
13:1
7:47
.29−1
1:21
:06.
215
.76
B90
677
8.10
30.
009
2W
D13
23− 5
1413
:26:
09.6
2−5
1:41
:37.
914
.60
L25
8−46
,L25
7−47
1935
722
7.76
50.
004
2H
E13
25−0
854
13:2
8:23
.90−0
9:09
:53.
015
.14
B17
021
167.
810
0.00
42
HE
1326−0
041
13:2
9:24
.69−0
0:56
:43.
916
.27
B18
671
557.
841
0.01
12
WD
1326−2
3613
:29:
24.9
2−2
3:52
:18.
115
.97
EC
1326
6−23
3613
808
857.
919
0.01
02
WD
1327−0
8313
:30:
13.5
8−0
8:34
:30.
212
.31
G01
4−05
8,B
D−0
7D36
3214
699
87.
791
0.00
13
HE
1328−0
535
13:3
1:20
.03−0
5:50
:52.
416
.34
B36
420
137
7.87
20.
020
2W
D13
28−1
5213
:31:
34.8
2−1
5:30
:48.
015
.49
EC
1328
8−15
15,H
E13
28−1
515
6125
328
57.
719
0.01
52
WD
1330+
036
13:3
3:17
.80+
03:2
1:00
.215
.86
GD
269,
BP
M89
123,
SD
SS
1740
826
7.83
10.
005
2W
D13
32−2
2913
:35:
10.4
7−2
3:10
:38.
316
.30
EC
1332
4−22
5520
264
497.
859
0.00
82
HS
1334+
0701
13:3
6:33
.67+
06:4
6:26
.815
.00
B16
891
437.
270
0.00
92
DD
sW
D13
34−1
6013
:36:
59.2
9−1
6:19
:44.
115
.32
EC
1334
2−16
04,L
0762−0
2118
653
218.
316
0.00
42
WD
1334−6
7813
:38:
08.1
1−6
8:04
:37.
415
.57
L10
6−73
,LH
S27
6987
698
7.92
90.
012
2H
E13
35−0
332
13:3
8:22
.72−0
3:47
:19.
516
.47
B20
188
758.
470
0.01
32
HS
1338+
0807
13:4
1:27
.63+
07:5
2:29
.516
.00
B24
440
188
7.64
90.
024
1H
E13
40−0
530
13:4
3:17
.88−0
5:45
:35.
816
.40
B32
936
141
7.91
10.
024
2W
D13
42−2
3713
:45:
46.5
8−2
3:57
:11.
016
.06
EC
1342
9−23
4210
988
198.
092
0.01
12
DA
VW
D13
44+
106
13:4
7:24
.45+
10:2
1:36
.615
.08
G06
3−05
4,L
HS
2800
6480
77.
079
0.01
52
WD
1348−2
7313
:51:
22.8
4−2
7:33
:59.
115
.00
LP
846−
53,L
TT
5382
9835
98.
039
0.00
83
WD
1349+
144
13:5
1:54
.06+
14:0
9:44
.215
.34
PG
1349+
114,
PB
4117
1692
528
7.64
20.
006
2D
Dd
WD
1356−2
3313
:59:
07.9
7−2
3:33
:28.
714
.96
EC
1356
3−23
1894
986
8.10
00.
007
2W
D14
01−1
4714
:03:
57.1
6−1
5:01
:10.
415
.67
EC
1401
2−14
4611
768
238.
080
0.00
82
DA
VW
D14
03−0
7714
:06:
04.8
6−0
7:58
:31.
015
.82
PG
1403−0
77,E
UV
EJ1
406−
07.9
4903
325
37.
810
0.01
72
WD
1410+
168
14:1
2:27
.89+
16:3
5:40
.515
.70
BL
P43
9−38
721
323
407.
756
0.00
72
HS
1410+
0809
14:1
3:06
.56+
07:5
5:23
.515
.50
B16
217
142
8.37
00.
020
2W
D14
11+
135
14:1
3:58
.22+
13:1
9:19
.316
.20
US
3969
1856
255
8.10
80.
011
2W
D14
12−1
0914
:15:
07.7
5−1
1:09
:24.
215
.86
mc
2622
652
7.81
40.
007
2H
E14
13+
0021
14:1
6:00
.21+
00:0
7:59
.316
.03
1454
481
8.11
40.
011
2H
E14
14−0
848
14:1
6:52
.07−0
9:02
:03.
816
.15
B98
237
7.86
70.
010
2D
Dd
452 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs
Tabl
e1.
cont
inue
d.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
WD
1418−0
8814
:20:
54.8
2−0
9:05
:08.
715
.36
G12
4−02
680
0310
7.91
10.
013
2W
D14
20−2
4414
:23:
26.2
5−2
4:43
:29.
416
.24
EC
1420
5−24
2920
917
408.
159
0.00
72
WD
1422+
095
14:2
4:39
.24+
09:1
7:12
.714
.32
GD
165,
L11
24−0
1012
525
217.
917
0.00
72
DA
VW
D14
26−2
7614
:29:
27.3
8−2
7:51
:01.
315
.92
EC
1426
5−27
3718
087
287.
661
0.00
62
HE
1429−0
343
14:3
2:03
.15−0
3:56
:37.
815
.84
B11
199
278.
041
0.01
52
DA
VH
S14
30+
1339
14:3
3:05
.47+
13:2
6:32
.416
.10
B10
012
128.
321
0.01
42
WD
1425−8
1114
:33:
08.9
2−8
1:20
:12.
613
.75
L19−2
,BP
M00
784
1206
917
7.91
60.
003
2D
AV
WD
1431+
153
14:3
4:06
.80+
15:0
8:17
.915
.80
BH
S14
31+
1521
,PG
1431+
153
1394
172
7.88
30.
008
2N
OV
(1)
HS
1432+
1441
14:3
5:20
.85+
14:2
8:41
.316
.00
BB
GK
,SD
SS
,GD
167
1620
442
7.74
80.
009
2W
D14
34−2
2314
:37:
14.7
4−2
2:31
:16.
016
.37
EC
1434
3−22
1827
690
138
7.37
40.
021
1H
E14
41−0
047
14:4
4:33
.85−0
0:59
:59.
516
.40
B(S
DS
S)
1577
572
8.02
50.
014
2N
OV
(3)
HS
1447+
0454
14:5
0:09
.91+
04:4
1:45
.715
.60
B13
926
387.
820
0.00
52
WD
1448+
077
14:5
0:49
.46+
07:3
3:32
.915
.46
G13
6−02
2,L
P56
1−01
314
921
307.
686
0.00
62
WD
1449+
168
14:5
2:11
.37+
16:3
8:03
.515
.44
PG
1449+
168
2234
646
7.78
50.
007
2W
D14
51+
006
14:5
3:50
.48+
00:2
5:29
.315
.19
GD
173,
GR
297,
SD
SS
2548
331
7.89
10.
004
2W
D14
57−0
8614
:59:
52.9
9− 0
8:49
:29.
515
.77
EC
1457
2−08
37,P
G14
57−0
8621
448
547.
917
0.00
92
WD
1500−1
7015
:03:
14.4
5−1
7:11
:56.
715
.27
EC
1500
4−17
0031
757
237.
926
0.00
52
WD
1501+
032
15:0
4:23
.92+
03:0
2:30
.515
.43
mc
PG
1501+
032
1474
150
7.93
20.
007
2W
D15
03−0
9315
:06:
19.4
4−0
9:30
:20.
915
.15
EC
1503
6−09
1812
681
208.
032
0.00
52
WD
1507+
220
15:0
9:39
.99+
21:5
0:15
.515
.00
BP
G15
07+
220
1987
227
7.74
50.
005
3W
D15
07+
021
15:0
9:56
.98+
01:5
6:07
.516
.49
PG
1507+
021,
SD
SS
2022
267
7.79
60.
012
1W
D15
07−1
0515
:10:
29.0
8−1
0:45
:19.
815
.42
GD
176
1006
38
7.66
30.
008
2N
OV
(1)
HE
1511−0
448
15:1
4:12
.97−0
4:59
:33.
915
.41
B(P
G15
11−0
48)
5089
912
67.
447
0.00
94
DD
sW
D15
11+
009
15:1
4:21
.31+
00:4
7:52
.315
.87
PG
1511+
009,
LB
769
2804
148
7.82
20.
009
2W
D15
15−1
6415
:18:
35.0
7−1
6:37
:29.
216
.03
EC
1515
7−16
2614
248
627.
969
0.00
32
HS
1517+
0814
15:2
0:06
.00+
08:0
3:27
.415
.90
BB
GK
,SD
SS
1449
444
7.76
10.
008
2H
E15
18−0
344
15:2
0:46
.03−0
3:54
:52.
216
.03
B28
493
507.
808
0.00
92
HE
1518−0
020
15:2
1:30
.87−0
0:30
:54.
715
.25
B15
392
297.
820
0.00
62
HE
1522−0
410
15:2
5:12
.26−0
4:21
:29.
316
.36
B10
357
128.
130
0.01
22
HS
1527+
0614
15:2
9:41
.47+
06:0
4:01
.915
.90
B14
925
397.
769
0.00
72
WD
1527+
090
15:2
9:50
.41+
08:5
5:46
.614
.29
PG
1527+
091
2119
727
7.84
60.
005
2W
D15
24−7
4915
:30:
36.6
4−7
5:05
:24.
215
.93
L72−9
1,B
PM
9518
2309
140
7.74
30.
006
3W
D15
31+
184
15:3
3:49
.31+
18:1
8:55
.416
.20
GD
186
1362
510
47.
774
0.01
31
NO
V(1
)W
D15
31−0
2215
:34:
06.0
8−0
2:27
:07.
314
.03
GD
185,
BP
M77
964
1923
418
8.35
40.
004
2W
D15
32+
033
15:3
5:09
.96+
03:1
1:13
.916
.02
PG
1532+
034
6190
732
77.
761
0.01
82
WD
1537−1
5215
:40:
23.7
7−1
5:23
:43.
215
.90
EC
1537
5−15
1416
954
297.
942
0.00
62
WD
1539−0
3515
:42:
14.1
5−0
3:41
:31.
415
.20
GD
189,
PG
1539−0
3598
756
8.24
60.
006
2W
D15
43−3
6615
:46:
58.2
3−3
6:46
:44.
115
.81
RE
1546−3
64,E
UV
EJ1
546−
367
4270
111
98.
974
0.01
22
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1544−3
7715
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30.0
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7:55
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812
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1−06
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547
58.
089
0.00
32
NO
V(1
)W
D15
47+
057
15:4
9:34
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05:3
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1547+
057
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47+
015
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9:44
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PG
1547+
016
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859
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22
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149
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246
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007
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183
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194,
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1470
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860
728.
248
0.00
72
NO
V(1
)W
D15
55−0
8915
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04.8
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9:08
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914
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2−B
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414
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627.
944
0.00
42
NO
V(1
)
D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs 453Ta
ble
1.co
ntin
ued. O
bjec
tR
A(2
000)
Dec
(200
0)m
ag(b
and)
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ases
Teff
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(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
WD
1609+
135
16:1
1:25
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13:2
2:17
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8−00
8,L
HS
3163
9256
68.
560
0.00
72
WD
1609+
044
16:1
1:49
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04:1
9:38
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PG
1609+
045
2959
322
7.79
10.
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1426
16:1
2:06
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14:1
9:05
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387
457.
821
0.00
83
WD
1614+
136
16:1
6:52
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PG
1614+
137
2201
530
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10.
005
2W
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14+
160
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7:08
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15:5
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BP
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28.0
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55.2
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957
0.00
72
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123
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2:03
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PG
1619+
123
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329
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33.8
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WD
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113
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00.7
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548
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683
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52
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225
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56.5
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44.8
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2289
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297.
837
0.00
52
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110
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218
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90.
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145
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172
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213
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42.0
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323
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19.6
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47.7
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314
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602
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WD
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46.9
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915
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7313
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407.
818
0.00
52
NO
V(1
)
454 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfsTa
ble
1.co
ntin
ued.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
WD
1952−5
8419
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12.9
9−5
8:20
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016
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HK
2287
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3350
961
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1519
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38.6
4−7
1:23
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615
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6,LT
T78
7519
267
257.
873
0.00
52
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059
20:0
2:12
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7:35
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226
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615
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1920
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17.4
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014
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30.
006
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56.8
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0:13
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712
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7987
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69
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7520
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54.8
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RE
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573
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28.7
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3:08
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414
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K22
955−
3715
585
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808
0.00
62
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2520
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59.5
7−4
2:24
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714
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RE
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424
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226
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005
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42.9
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2:41
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183
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2:02
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230
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577
7.64
70.
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(1)
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188
20:3
5:13
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9:21
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231,
BP
M95
701
1819
928
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50.
005
2D
Ds
WD
2039−2
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34.6
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0:04
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8189
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738
107.
786
0.00
22
WD
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21.3
5−6
8:05
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413
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6−79
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9016
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128.
336
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HS
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0044
20:4
8:38
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00:5
6:00
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B27
096
328.
153
0.00
53
WD
2046−2
2020
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46.1
8−2
1:54
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115
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HK
2288
0−12
423
413
377.
828
0.00
52
WD
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095
20:5
3:43
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09:4
1:14
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BL
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S20
51+
0929
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430
7.79
00.
007
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8:45
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07:3
3:37
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289
428.
321
0.00
71
WD
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033
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8:46
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1:49
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PG
2056+
033
5183
525
27.
696
0.01
62
HS
2058+
0823
21:0
1:13
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08:3
5:09
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00.
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181
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0:55
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GD
232,
GR
279
1734
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7.75
40.
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3H
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547.
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WD
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190
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969
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HS
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1734
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6:32
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90.
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010
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7:33
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PG
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011
2581
539
7.75
50.
005
2W
D21
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6021
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36.6
0−5
5:50
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614
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2−19
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273
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011
0.00
72
WD
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054
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2:34
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05:4
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PG
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055
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10.
011
2W
D21
22−4
6721
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30.1
9−4
6:30
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816
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BH
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643
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8.05
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2421
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43.2
1−2
2:11
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914
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4778
014
97.
707
0.01
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HS
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21:3
3:01
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12:2
8:30
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BS
DS
S32
995
897.
738
0.01
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HS
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0941
21:3
4:50
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09:5
5:19
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204
717.
720
0.00
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HE
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332
21:3
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60.
005
2W
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218
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227
1800
119
7.86
40.
004
2W
D21
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8:46
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23:0
9:20
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582
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411
8.06
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009
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OV
(1)
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2135−4
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21:3
8:49
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0:41
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913
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B(N
LTT
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3)19
211
177.
959
0.00
32
WD
2137−3
7921
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18.4
8−3
7:42
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716
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BH
E21
37−3
756
2101
346
7.85
50.
008
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21:4
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09:2
3:45
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637
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30.
010
2W
D21
39+
115
21:4
1:28
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11:4
6:22
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GD
235,
GR
280
1555
128
7.79
40.
007
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825
21:4
3:42
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8:11
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616
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950
397.
751
0.00
62
WD
2146−4
3321
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38.9
6−4
3:06
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415
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HK
2295
1−67
6279
238
87.
230
0.02
02
HS
2148+
1631
21:5
1:14
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16:4
5:23
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B16
776
347.
793
0.00
72
HE
2148−3
857
21:5
1:19
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8:43
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516
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758
968.
015
0.01
41
WD
2149+
021
21:5
2:25
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02:2
3:17
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G09
3−04
8,E
G15
017
926
97.
862
0.00
22
WD
2150+
021
21:5
3:30
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02:2
3:11
.616
.40
PG
2150+
021
4087
415
87.
659
0.01
62
WD
2152−0
4521
:54:
41.1
8−0
4:18
:18.
015
.00
BH
K22
965−
2019
837
367.
380
0.00
63
WD
2151−3
0721
:54:
53.3
8−3
0:29
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614
.82
BR
E21
54−3
02,E
UV
EJ2
154−
304
2858
026
8.27
30.
005
2
D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs 455Ta
ble
1.co
ntin
ued.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
WD
2152−5
4821
:56:
21.3
2−5
4:38
:24.
114
.50
4517
112
17.
878
0.00
92
WD
2153−4
1921
:56:
35.3
2−4
1:42
:17.
015
.89
HE
2153−4
156,
RE
J215
6−41
446
503
177
7.93
90.
015
2W
D21
54−0
6121
:57:
29.9
2−0
5:51
:54.
815
.10
BH
K22
965−
8,P
B70
2636
259
857.
744
0.01
22
HE
2155−3
150
21:5
8:46
.08−3
1:36
:06.
516
.06
B16
302
407.
833
0.00
92
WD
2157+
161
21:5
9:34
.35+
16:2
5:39
.016
.20
GD
272,
GR
282
1918
831
7.88
90.
006
3H
E21
59−1
649
22:0
2:20
.82−1
6:34
:38.
315
.90
B19
486
347.
841
0.00
62
WD
2159−4
1422
:02:
28.5
7−4
1:14
:30.
615
.88
HE
2159−4
129,
EU
VE
J220
2−41
.254
343
219
7.70
70.
015
2W
D22
00−1
3622
:03:
35.6
3−1
3:26
:49.
915
.36
HE
2200−1
341
2473
447
7.61
10.
006
2D
Dd
WD
2159−7
5422
:04:
21.2
7−7
5:13
:25.
915
.06
LH
S35
72,B
PM
1452
589
116
8.62
20.
008
2H
E22
03−0
101
22:0
6:02
.44−0
0:46
:33.
515
.82
B(P
B50
70)
1804
733
7.87
10.
007
2W
D22
04+
071
22:0
7:16
.20+
07:1
8:36
.015
.86
PG
2204+
071
2445
439
7.95
00.
005
3W
D22
05−1
3922
:08:
29.6
0−1
3:41
:13.
215
.08
HE
2205−1
355
2523
132
8.24
60.
004
3W
D22
07+
142
22:0
9:47
.19+
14:2
9:46
.615
.61
G01
8−03
4,LT
T16
482
7229
207.
603
0.03
22
HE
2209−1
444
22:1
2:18
.05−1
4:29
:48.
015
.32
BK
awka
06,N
LTT
5317
782
900
8.19
10.
030
1D
Dd
HS
2210+
2323
22:1
2:53
.48+
23:3
8:00
.415
.70
B23
233
478.
238
0.00
62
WD
2211−4
9522
:14:
11.9
3−4
9:19
:27.
111
.70
RE
2214−4
91,E
UV
EJ2
214−
493
6233
618
17.
544
0.00
72
HS
2216+
1551
22:1
8:57
.15+
16:0
6:56
.915
.70
B17
112
297.
872
0.00
62
DD
dH
E22
18−2
706
22:2
1:23
.91−2
6:50
:55.
214
.89
B15
039
307.
795
0.00
52
HE
2220−0
633
22:2
2:44
.44−0
6:17
:54.
915
.97
B(P
HL
243)
1552
338
7.88
50.
007
2H
S22
20+
2146
B22
:23:
01.6
4+
22:0
1:31
.015
.00
B18
743
448.
241
0.00
82
HS
2220+
2146
A22
:23:
01.7
4+
22:0
1:25
.015
.00
B14
601
328.
080
0.01
21
WD
2220+
133
22:2
3:13
.95+
13:3
8:55
.515
.60
PG
2220+
134,
SD
SS
2258
329
8.29
90.
005
3H
E22
21−1
630
22:2
4:17
.51−1
6:15
:47.
016
.18
B(P
HL
5103
)99
379
8.16
10.
008
2H
S22
25+
2158
22:2
8:11
.47+
22:1
4:15
.115
.30
B25
989
437.
856
0.00
62
WD
2226+
061
22:2
9:08
.66+
06:2
2:46
.314
.70
GD
236,
LP
580−
021
1642
929
7.65
50.
006
2W
D22
26−4
4922
:29:
19.4
7−4
4:41
:39.
415
.50
HK
2296
0−99
1392
321
7.74
30.
003
3H
S22
29+
2335
22:3
1:45
.45+
23:5
1:23
.915
.60
B19
300
387.
900
0.00
72
HE
2230−1
230
22:3
3:38
.69−1
2:15
:30.
416
.08
B(P
HL
315,
GD
237)
2094
941
7.80
70.
007
2H
E22
31−2
647
22:3
4:02
.59−2
6:32
:21.
114
.96
B21
592
417.
700
0.00
62
HS
2233+
0008
22:3
6:03
.20+
00:0
7:23
.913
.90
B(P
HL
329)
2452
922
7.98
90.
003
2W
D22
35+
082
22:3
7:35
.56+
08:2
8:48
.515
.42
PG
2235+
082
3651
949
7.73
40.
007
4H
E22
38−0
433
22:4
1:04
.90−0
4:18
:09.
114
.30
B(P
HL
372)
1754
211
68.
178
0.02
32
HS
2240+
125B
22:4
2:30
.33+
12:5
0:02
.216
.50
B13
935
112
7.98
90.
012
2H
S22
40+
125A
22:4
2:31
.14+
12:5
0:04
.716
.20
B15
636
97.
857
0.00
82
WD
2240− 0
4522
:42:
44.6
2−0
4:14
:15.
115
.21
GD
240,
FE
IGE
106
4410
210
77.
721
0.01
02
WD
2240−0
1722
:43:
04.7
6−0
1:27
:53.
616
.17
G02
8−01
3,P
HL
386
9114
108.
050
0.01
32
WD
2241−3
2522
:44:
43.2
3−3
2:19
:43.
715
.97
BH
E22
41−3
235,
PH
L39
632
316
327.
945
0.00
72
HS
2244+
2103
22:4
6:45
.28+
21:1
9:47
.715
.70
B24
113
607.
889
0.00
82
HS
2244+
0305
22:4
7:22
.35+
03:2
1:45
.816
.20
B(P
B51
60)
6046
041
37.
540
0.02
32
HE
2246−0
658
22:4
8:40
.05−0
6:42
:44.
214
.14
B(P
B72
25)
1137
150
8.18
60.
021
WD
2248−5
0422
:51:
02.0
2−5
0:11
:31.
814
.96
L28
5−14
,BP
M28
016
1633
637
7.73
70.
007
2H
E22
51−6
218
22:5
4:59
.62−6
2:02
:10.
215
.89
B18
033
447.
827
0.00
92
WD
2253−0
8122
:55:
49.4
9−0
7:50
:03.
316
.50
G15
6−06
4,B
D−0
8◦59
80B
6211
136.
926
0.02
63
WD
2254+
126
22:5
6:46
.26+
12:5
2:49
.916
.00
BG
D24
4,L
P52
1−04
911
707
237.
989
0.00
93
DA
V
456 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs
Tabl
e1.
cont
inue
d.
Obj
ect
RA
(200
0)D
ec(2
000)
mag
(ban
d)A
lias
esT
eff[K
]σ
(Teff
)[K
]lo
ggσ
(logg)
Spe
ctra
Rem
arks
HS
2259+
1419
23:0
1:55
.18+
14:3
6:00
.515
.80
BB
GK
,SD
SS
1381
657
7.74
30.
007
212
672
307.
821
0.00
92
amb
WD
2303+
017
23:0
6:13
.09+
01:5
8:51
.615
.76
BP
G23
03+
017,
PH
L40
040
977
112
7.66
70.
011
3W
D23
03+
242
23:0
6:17
.70+
24:3
2:07
.515
.29
PG
2303+
243,
KR
Peg
1114
711
8.01
80.
006
2D
AV
WD
2306+
130
23:0
8:30
.58+
13:1
9:22
.715
.10
PG
2306+
131,
KU
V23
060+
1303
1351
351
7.82
60.
006
2N
OV
(1)
WD
2306+
124
23:0
8:35
.07+
12:4
5:39
.015
.23
PG
2306+
125,
KU
V23
061+
1229
2036
038
7.99
30.
006
2W
D23
08+
050
23:1
1:18
.05+
05:1
9:27
.916
.02
PG
2308+
050,
PB
5280
3606
268
7.60
60.
010
2W
D23
09+
105
23:1
2:21
.71+
10:4
7:02
.813
.00
GD
246,
BP
M97
895
5700
713
67.
816
0.00
72
WD
2311−2
6023
:13:
53.2
0−2
5:48
:49.
016
.05
BG
D16
36,T
ON
S09
451
160
332
7.77
20.
021
2W
D23
12−3
5623
:15:
34.9
5−3
5:24
:51.
815
.20
BH
K22
888−
3215
122
217.
818
0.00
43
WD
2314+
064
23:1
6:50
.36+
06:4
1:27
.615
.93
mc
PG
2314+
064,
PB
5312
1798
130
7.87
50.
006
2H
E23
15−0
511
23:1
8:04
.31−0
4:54
:45.
715
.37
B(P
HL
444)
3345
182
7.72
10.
014
3W
D23
18+
126
23:2
0:31
.30+
12:5
8:14
.516
.10
BH
S23
18+
1241
,LP
582−
4113
788
597.
803
0.00
82
WD
2318−2
2623
:21:
26.4
3−2
2:20
:22.
516
.05
GD
1648
,PH
L47
529
851
507.
890
0.01
12
WD
2321−5
4923
:24:
30.8
5−5
4:41
:35.
515
.20
HE
2321−5
458,
RE
J232
4−54
443
583
947.
783
0.00
82
WD
2322+
206
23:2
4:35
.22+
20:5
6:33
.915
.59
PG
2322+
207,
HS
2322+
2040
1263
628
7.84
20.
006
2N
OV
(1)
WD
2322−1
8123
:25:
18.4
0−1
7:51
:57.
815
.38
BG
273−
040,
LP
822−
081
2168
335
7.90
00.
006
2W
D23
24+
060
23:2
6:44
.55+
06:1
7:41
.415
.33
mc
PG
2324+
060,
PB
5379
1626
120
7.82
70.
005
2W
D23
26+
049
23:2
8:47
.74+
05:1
4:53
.513
.10
G02
9−03
8,LT
T16
907
1148
58
8.07
10.
002
2D
AV
WD
2328+
107
23:3
0:41
.79+
11:0
2:05
.015
.53
PG
2328+
108,
KU
V23
282+
1046
2239
030
7.77
80.
004
2W
D23
29−3
3223
:32:
10.9
0−3
3:01
:08.
116
.26
BH
E23
29−3
317,
GD
1670
2045
770
7.91
40.
012
2W
D23
30−2
1223
:32:
59.4
8−2
0:57
:12.
116
.25
BH
E23
30−2
113,
PH
L55
926
442
697.
443
0.01
02
DD
sW
D23
31−4
7523
:34:
02.3
2−4
7:14
:27.
613
.42
RE
2334−4
71,E
UV
EJ2
334−
472
5157
394
7.87
50.
006
2W
D23
33−1
6523
:35:
36.5
9−1
6:17
:42.
513
.80
BG
D11
92,B
PM
8275
813
303
197.
875
0.00
32
WD
2333−0
4923
:35:
53.9
6−0
4:42
:14.
815
.65
G15
7−08
210
608
128.
040
0.00
92
NO
VH
E23
34−1
355
23:3
7:30
.38−1
3:38
:33.
415
.64
B(G
D12
07,P
B77
13)
3049
827
7.28
80.
006
2W
D23
36−1
8723
:38:
52.7
8−1
8:26
:11.
915
.60
PG
273−
097,
GR
557
7774
97.
492
0.01
42
DD
dW
D23
36+
063
23:3
8:58
.25+
06:3
5:28
.615
.60
mc
PG
2336+
063,
PB
5486
1701
220
8.02
50.
004
2M
CT
2343−1
740
23:4
6:25
.63−1
7:24
:10.
216
.12
BG
D13
2421
827
104
7.88
30.
015
2H
E23
45−4
810
23:4
7:46
.16−4
7:53
:42.
815
.99
B29
352
357.
324
0.00
72
DD
sM
CT
2345−3
940
23:4
8:26
.42−3
9:23
:47.
416
.06
B19
197
467.
866
0.00
82
WD
2347+
128
23:4
9:53
.51+
13:0
6:12
.516
.05
G03
0−02
0,G
R40
510
874
197.
999
0.01
12
DA
VW
D23
47−1
9223
:50:
02.9
6−1
8:59
:21.
916
.03
MC
T23
47−1
916,
GD
1248
2627
249
7.94
10.
007
2H
E23
47−4
608
23:5
0:32
.90−4
5:51
:34.
816
.20
B17
738
337.
304
0.00
72
WD
2348−2
4423
:51:
22.1
0−2
4:08
:17.
015
.33
EC
2348
7−24
2411
406
148.
040
0.00
62
DA
VM
CT
2349−3
627
23:5
2:08
.16−3
6:10
:40.
116
.41
B44
455
265
7.87
70.
022
2W
D23
49−2
8323
:52:
23.1
8−2
8:03
:15.
915
.54
BM
CT
2349−2
819,
PH
L57
817
427
247.
730
0.00
52
WD
2350−2
4823
:53:
03.7
9−2
4:32
:03.
115
.21
BM
CT
2350−2
448,
PH
L58
028
867
268.
375
0.00
52
WD
2350−0
8323
:53:
27.6
3−0
8:04
:39.
516
.18
mc
G27
3−B
1B,G
R55
818
529
377.
790
0.00
72
WD
2351−3
6823
:54:
18.8
2−3
6:33
:55.
115
.10
BL
505−
42,L
P93
6−02
514
438
287.
869
0.00
52
MC
T23
52−1
249
23:5
5:13
.68−1
2:32
:55.
116
.49
PH
L58
4,P
B80
9840
294
351
7.95
20.
040
2W
D23
53+
026
23:5
6:27
.70+
02:5
7:06
.015
.83
PG
2353+
027,
PB
5617
6174
028
67.
590
0.01
62
WD
2354−1
5123
:57:
33.4
4−1
4:54
:09.
115
.02
BM
CT
2354−1
510,
PH
L59
934
984
407.
195
0.00
72
HE
2356−4
513
23:5
8:57
.83−4
4:57
:13.
515
.38
B17
418
177.
861
0.00
43
D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs 457
0.50
1.00
1.50
2.00
HE1124+0144 16221 7.76
0.50
1.00
1.50
2.00
WD1124-293 9476 8.09
0.50
1.00
1.50
2.00
WD1124-018 24325 7.54
0.50
1.00
1.50
2.00
WD1125-025 31819 8.16
-100.0 -50.0 0.0 50.0 100.0
0.50
1.00
1.50
2.00
Δ λ [Α]
WD1125+175 61488 7.57
WD1126-222 12032 7.93
WD1129+071 14297 7.84
WD1129+155 17712 8.03
WD1130-125 14468 8.25
-100.0 -50.0 0.0 50.0 100.0
Δ λ [Α]
HS1136+1359 23920 7.83
Fig. 1. Typical example for observations and fit, taking arbitrarily the entries 301 to 310 from Table 1. The header of each panel gives the name,effective temperature, and surface gravity of the fit. Shown are the six lowest Balmer lines. Vertical axis is relative intensity in arbitrary units,higher lines are offset for clarity. The light grey lines are the models.
of Liebert et al. (2005), the remaining standard deviations areσ(Teff) = 2.3%, and σ(log g) = 0.08. These values should betaken as indicative of the statistical errors of our results, and arecompatible with the estimates derived above for the internal un-certainties from multiple spectra within our sample.
The surprisingly large systematic shift in surface grav-ity is unsatisfactory. A similar trend was also noted byLiebert et al. (2005) in their comparison with studies by otherauthors. In four out of five cases their log g was higher by0.06−0.10 dex. Three of these used similar models to those used
458 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs
10000. 15000. 20000. 25000. 30000. 35000. 40000. 45000.
10000.
15000.
20000.
25000.
30000.
35000.
40000.
45000.
Teff [K]
Tef
f [K
] (L
BH
)
Fig. 2. Comparison of effective temperatures from this work with theresults of Liebert et al. (2005), (=LBH) for 85 objects in common.
7.25 7.50 7.75 8.00 8.25 8.50 8.75
7.25
7.50
7.75
8.00
8.25
8.50
8.75
log g
log
g (L
BH
)
Fig. 3. Comparison of surface gravities from this work with the resultsof Liebert et al. (2005), (=LBH) for 85 objects in common.
here, and the differences could arise from differences betweenthe “Bergeron” and the “Koester” models, or from the fittingprocedures used. We are, however, not aware of any obviousexplanations for such differences. Systematic differences of thismagnitude were also found by Napiwotzki et al. (1999) in a com-parison of different studies using low-resolution spectra.
A possible reason for systematic differences may also comefrom the nature of our observational data. The main purpose ofthe SPY was the determination of radial velocities, which neededhigh resolution; therefore the echelle spectrograph UVES wasused. The wavelength interval per order ranges from ≈30 Å inthe blue to ≈50 Å in the red region. Thus, e.g. Hα at maximumstrength will extend over six or more orders, which have to beflatfielded and merged, removing the strong sensitivity changewithin orders. A real flux calibration was not possible, but thequality of the spectra obtained after some reprocessing of theESO pipeline results was still very impressive. Before the startof this project, we were not certain that the spectra would beuseful for anything else except radial velocity determinations.
Nevertheless, the merging of the orders and the approximateflux calibration attempted may have left very subtle artifacts in-fluencing the far wings of the strong lines, thus influencing inparticular the surface gravity results. An indication for this isvisible in Table 1 in Koester et al. (2001), which compares theresults of fits to echelle vs. single-order low-resolution spectra
for the same seven DAs. The average surface gravity is lower by0.07 in the results from the echelle spectra. Another hint towardsthis effect can be found in the study of low-resolution SDSSspectra of brighter DA white dwarfs by Koester et al. (2009),which used the same models and fitting routines as this work.The average surface gravity for 578 DAs with magnitude g < 19,S/N > 10, and 8000 K ≤ Teff ≤ 16 000 K is 8.014, while the valuefrom our current sample for the same temperature range is 7.947from 211 objects. These are not the same objects of course, butthe samples are so large, that the difference is significant.
Also marked in Table 1 are known ZZ Ceti variables (DAV),as well as objects, which have been observed photometrically,but were not found to vary (NOV). The references for the NOVdesignations are: (1) Gianninas et al. (2005); (2) Kepler et al.(1995); (3) Mukadam et al. (2004); and (4) Bergeron et al.(2004). If no reference is given the classification is a result ofthe SPY and/or follow-up observations (Voss 2006; Voss et al.2006; Castanheira et al. 2006; Silvotti et al. 2005). We have notmarked candidates for variability studies, but obviously all ob-jects in the range of Teff 10 000−13 000 K are interesting in thisrespect.
The Balmer lines reach their maximum strength near Teff =13 000, the exact value depending on the surface gravity.Therefore quite often two different fitting solutions exist, whichproduce the same overall strength (i.e. equivalent width) of thelines. The χ2 values of the two minima are often similar, sincemodel and observation are fitted in the far line wings and dif-ferences show up only in the inner core of the line. Visual in-spection is usually sufficient to determine the correct solution.In a few cases, however, the difference was so small that we pre-ferred to give both solutions in Table 1.
Because of the selection of the targets – as mentioned in theintroduction – our sample is not well suited for a study of whitedwarf population characteristics such as the mass distribution.However, it can be used to demonstrate an effect well known formany years (Bergeron et al. 1990a; Bergeron 1992; Kleinmanet al. 2004; Eisenstein et al. 2006; Kepler et al. 2007; DeGennaroet al. 2008; Koester et al. 2009). This is the fact that the sur-face gravity seems to increase around Teff ≈ 12 000 K towardslower temperatures. Figure 4 clearly shows this for 465 objectsbetween 7500 and 25 000 K. Taking the direct averages withoutany weighting we find 〈log g〉 = 7.86 for effective temperaturesabove 12 500 K and 〈log g〉 = 8.06 below. This is very similar tothe results in the SDSS (Data Release 4) as studied by Koesteret al. (2009). A number of possible explanations is discussed inthat study, and the most likely is found to be an inadequate de-scription of convection with the mixing-length approximation.However, this problem is certainly not yet solved.
4. Double-degenerate white dwarfs
Two or more spectra were taken for the vast majority of theSPY targets. Close binaries among them could be detected witha high level of confidence by checking for radial velocity vari-ations indicating orbital motion. A total of 36 close binarieswere detected among DA sample presented here from the spec-tra taken for the SPY. This count includes only the doubledegenerates, i.e. systems consisting of two white dwarfs. TheDA+dM systems listed in Table 3 are not included in this count.Seventeen of the double-degenerates are double-lined, i.e. spec-tral lines of both white dwarfs are present in the spectra. Thewhite dwarf companion in the single-lined systems is already socool and faint that it does not produce a significant contributionto the combined spectrum.
D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs 459
Table 2. Magnetic or helium-contaminated hydrogen-rich stars.
Object RA(2000) Dec(2000) mag(band) Aliases RemarksWD 2359−434 00:02:10.73 −43:09:55.3 13.05 L362−81, LHS 1005 DAPHS 0051+1145 00:54:18.25 +12:01:59.9 15.60 (PHL 886) DAHWD 0058−044 01:01:02.25 −04:11:11.2 15.38 GD 9, GR 407 DAHHS 0209+0832 02:12:04.90 +08:46:50.1 13.90 DABWD 0239+109 02:42:08.54 +11:12:31.8 16.18 G 004−034, LTT 10886 DAHWD 0257+080 02:59:59.24 +08:11:55.3 15.90 LHS 5064, G 76−48 DAHHS 1031+0343 10:34:30.14 +03:27:36.0 16.50 B DAHHE 1233−0519 12:35:37.58 −05:35:36.7 16.48 DAHWD 1953−011 19:56:29.21 −01:02:32.2 13.69 G 092−040, L 0997−021 DAHWD 2051−208 20:54:42.76 −20:39:25.9 15.06 HK 22880−134 DAHWD 2105−820 21:13:16.52 −81:49:14.3 13.50 L 24−52, LTT8381 DAH
10000.12500.15000.17500.20000.22500.
7.25
7.50
7.75
8.00
8.25
8.50
8.75
Teff [K]
log
g
Fig. 4. Distribution of surface gravities for all objects between Teff
7500−25 000 K.
Four more double-degenerates are marked in Table 1 asDD, but were found by independently obtained observations:HE 1511-0448 (Nelemans et al. 2005), WD 1241-010 (Marshet al. 1995), WD 1022+050 and WD 2032+188 (Morales-Ruedaet al. 2005).
The fitting procedure for the model atmosphere analysis isnot affected by the binary nature of the single-lined binaries. Theresulting fit parameters are those of the visible bright component.The situation is different for the double-lined systems. In thesecases a deconvolution of simultaneous fit of both componentswould be necessary for accurate parameters. We have tools forthis kind of analysis available (Napiwotzki et al. 2004), but inmost cases more than the two spectra taken during the survey areneeded to derive reliable parameters of both components. Herewe present the results of a fit assuming a single star. Althoughthese have to be taken with a pinch of salt, they are still a usefulindication of the nature of properties of the binary. Double-linedsystems are indicated in Table 1.
5. Objects with magnetic fields or heliumcontamination
Table 2 summarizes the data for some objects, which appearhydrogen-rich with some peculiarities, either Zeeman splittingof the Balmer lines due to a magnetic field or helium lines inaddition to the stronger Balmer lines. For most of the stars weobtained fits with pure hydrogen model atmospheres. Since theseare obviously not very reliable, we do not publish the parametershere, but discuss these stars individually.
Four magnetic DA stars in the SPY sample havenot been published before, HS 0051+1145, HE 1233−0519,HS 1031+0343, and WD 2051−208. Two more objects werepublished first as DAH stars in Koester et al. (2001),WD 0058−044 and WD 0239+109. Four more magnetic DA, al-ready described in the literature, are in the sample. Below, theseten objects and some additional white dwarfs of special interestare discussed.
HS 1031+0343. This object is a new magnetic DA star. Theonly Zeeman triplet that is completely present, and for whichthe three components are well discernible, is that of Hβ. The σ−,π, σ+ components are found at 4771 Å, 4851 Å, and 4905 Å.The components of the higher lines are blended together, andthe σ+ component of Hα is shifted by an amount that placesit outside of the observed spectral range; thus only the σ− andπ components of Hα are available in the SPY data, at 6560 Å and6420 Å. The magnetic field is estimated as B = 6.1 ± 0.3 MG.
WD 0058−044. This star has been published as a magnetic DAby Koester et al. (2001). The shifts of the σ components withrespect to the π components are 6.2 ± 0.3 Å and 3.6 ± 0.3 Å, forHα and Hβ, respectively. The components of the higher Balmerlines are blended. The quadratic splitting of the lines is negligi-ble here since the split is small and thus the field strength has tobe low. The field is B = 330 ± 30 kG, from Hα, and B = 310 ±20 kG, from Hβ.
WD 0239+109. Greenstein & Liebert (1990) recognized an un-usual line shape for this object, and suggested a magnetic fieldas one of the possible reasons. Bergeron et al. (1990b) inter-preted the spectrum as that of an unresolved DA+DC binary.The SPY spectra in Koester et al. (2001) revealed the presenceof Zeeman splitting of Hα and thus proved the magnetic natureof the object. In the first SPY spectrum, the Hα components areplaced at 6576.6 Å, 6562.3 Å, and 6548.4 Å, and those of Hβat 4868.9 Å, 4861.0 Å, 4853.0 Å, and from that field strengthsof 700 ± 20 kG, from Hα, and 720 ± 30 kG, from Hβ, can bederived.
WD 0257+080. Bergeron et al. (1997) found a flat-bottomHα core for this object which is typical for white dwarfs witha low-strength magnetic field, but they were not able to identifya Zeeman triplet and estimated the field strength to be ∼100 kG.One of the two SPY spectra of WD 0257+080 clearly shows anHα triplet. In the other spectrum, which has a slightly lower S/N,
460 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs
Table 3. Data for DA+dM binaries. In boldface are the new SPY detections. For explanations of the magnitude column see text.
Object RA(2000) Dec(2000) mag(band) Aliases TypeHE 0016−4340 00:19:06.10 −43:24:18.5 15.62 B DA2WD 0034−211 00:37:24.99 −20:53:43.6 14.53 MCT 0034−2110, LP 852−559 DA3HE 0105−0232 01:08:06.33 −02:16:53.1 15.77 B (PB6272) DA2WD 0131−163 01:34:24.08 −16:07:08.2 13.98 MCT 0131−1622, PHL 1043 DA1WD 0137−349 01:39:42.88 −34:42:39.1 15.33 HK 29504−36 DA3WD 0205+133 02:08:03.59 +13:36:23.9 13.78 B PG 0205+134 DA1WD 0232+035 02:35:07.67 +03:43:55.6 12.25 Feige 24 DA1WD 0303−007 03:06:07.21 −00:31:14.3 16.21 HE 0303−0042, KUV 03036−0043 DA2WD 0308+096 03:10:54.90 +09:49:31.6 15.23 PG 0308+096 DA2HE 0331−3541 03:33:52.53 −35:31:18.9 14.79 B DA2WD 0347−137 03:50:14.55 −13:35:13.5 14.00 GD 51, LP 713−034 DA3HE 0409−3233 04:11:21.14 −32:26:14.9 16.03 B DA3WD 0429+176 04:32:23.76 +17:45:02.4 13.93 GH 7−255, HZ9B DA3WD 0430+136 04:33:10.59 +13:45:12.4 16.50 KUV 04304+1339 DA1HE 0523−3856 05:25:28.11 −38:54:12.5 16.07 B DA3WD 0718−316 07:20:47.92 −31:47:04.6 15.10 RE 0720−314, EUVE J 0720−317 DAOWD 0933+025 09:35:40.69 +02:21:59.6 16.01 B PG 0933+026 DA2WD 0950+185 09:52:45.80 +18:21:02.9 15.30 PG 0950+186 DA2WD 1001+203 10:04:04.30 +20:09:22.5 15.35 TON 1150, HS1001+2023 DA2WD 1026+002 10:28:34.88 −00:00:29.6 13.89 B PG 1026+002, HE 1026+014 DA3WD 1042−690 10:44:10.63 −69:18:22.9 13.09 BPM 06502, L 101−080 DA2WD 1049+103 10:52:27.82 +10:03:36.5 15.83 B PG 1049+103 DA3HE 1103−0049 11:06:27.66 −01:05:14.9 16.30 B DA3HE 1208−0736 12:11:01.08 −07:52:42.9 15.67 B DA2WD 1247−176 12:50:22.13 −17:54:48.2 16.19 EC 12477−1738, HE 1247−1738 DA3WD 1319−288 13:22:40.46 −29:05:35.0 15.99 EC 13198−2849 DA5HE 1333−0622 13:36:19.64 −06:37:58.9 16.05 WD 1333−063 DA2WD 1334−326 13:37:50.77 −32:52:22.5 16.34 EC 13349−323 DA1HE 1346−0632 13:48:48.34 −06:47:21.0 16.27 B DA2EC 13471−125 13:49:51.95 −13:13:37.5 14.80 WD 1347−129, RXS DA3WD 1415+132 14:17:40.22 +13:01:48.6 15.29 US 3974, Feige 93 DA1EC 14329−162 14:35:45.70 −16:38:17.0 14.89 WD 1432−164, HE 1432−1625 DA3WD 1436−216 14:39:12.70 −21:50:14.6 15.94 EC 14363−2137, HE 1436−2137 DA2WD 1458+171 15:00:19.36 +16:59:14.7 16.12 B PG 1458+172 DA5WD 1541−381 15:45:10.97 −38:18:51.3 14.90 LDS 539B, L 480−085 DA4HS 1606+0153 16:08:55.22 +01:45:48.6 15.00 B DA3WD 1643+143 16:45:39.05 +14:17:42.0 15.38 PG 1643+144 DA2WD 1646+062 16:49:07.83 +06:08:43.6 15.84 B PG 1646+062 DA2WD 1845+019 18:47:39.09 +01:57:33.5 12.95 LAN 18, KPD 1845+0154 DA2WD 1844−654 18:49:02.00 −65:25:14.2 15.80 B HK 22959−81 DA1HS 2120+0356 21:23:09.53 +04:09:28.3 16.20 B DA3HE 2123−4446 21:26:41.88 −44:33:38.8 15.97 B DA3HE 2147−1405 21:50:03.69 −13:51:45.9 15.94 B (PHL 167) DA2WD 2151−015 21:54:06.53 −01:17:10.9 14.41 G 093−053,L 1003−016 DA2HE 2217−0433 22:20:05.80 −04:18:44.5 16.28 B DA3WD 2313−330 23:16:02.90 −32:46:41.4 15.74 B HK 22888−45, MCT DA1
only the σ− component is discernible. The Hα components ofthe first spectrum are split by 1.8 ± 0.3 Å, from which B = 90 ±15 kG can be derived, a more precise value than the previousestimate.
WD 1953−011. A weak Zeeman-split triplet of Hα was foundby Koester et al. (1998), from which they derived a field strengthof 93 kG. Maxted et al. (2000) had noticed a variable depressionin the wings of Hα which they identified as additional Zeeman-split Hα features, which led them to assume a non-simple fieldgeometry with a strong spot-like field of ∼500 kG combinedwith a weaker 70 kG dipole field. Comparing the two SPY spec-tra, the Hα wings appear deformed near 6550 Å and 6575 Å,which might allow a very rough estimate of field strengths of∼500 kG up to ∼750 kG, if it is assumed that these features areof magnetic origin. However no variation of these features as
described by Maxted et al. can be found, the line shape is verysimilar in both SPY spectra. The central triplet however is obvi-ous, and the splitting of the core is 1.9 ± 0.2 Å. This correspondsto a dipole B field of 95 ± 10 kG.
WD 2105−820. The spectrum of this star was found to show aflat-bottom Hα core, probably due to a low magnetic field, byKoester et al. (1998), from which they derive a field strength of43 kG. No Zeeman triplet is obvious in the SPY spectra as well,they also only exhibit the broadened, flat core; the full width ofthe core of 1.8 Å in the SPY spectra is consistent with the fieldstrength derived by Koester et al. (1998).
WD 2359−434. Koester et al. (1998) suspected that this DAcould be magnetic due to its flat Hα core, and a very low field
D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs 461
of only 3 kG was polarimetrically found by Aznar Cuardradoet al. (2004). They selected this object as one of their programstars based on the criterion that the SPY spectra show no signs ofZeeman splitting; however they themselves note that flat Balmerline cores are present in the spectra of that object, and if theseare caused by the B field, it would indicate a higher field strengththan that derived from the polarimetry data. Kawka et al. (2007)measure a low field of 3.4 ± 4.4 kG.
The SPY spectra indeed do not only show a flat-bottomHα core, but within that core also a pronounced π compo-nent and less clear, broad σ components, centered at 6561.1 Å,6563.5 Å, and 6565.8 Å. Thus a field strength of 110± 10 kG canbe derived. This is two orders of magnitude stronger than foundby Aznar Cuardrado et al. (2004) and Kawka et al. (2007). Thereason for these different results is unclear.
WD 0446−789 and WD 1105−048. These objects are the tworemaining of the three for which Aznar Cuardrado et al. (2004)discovered magnetic fields of only a few kG from polarimetrydata. The Hα core of WD 0446−789 appears slightly broadened,the width is 1.8 Å, which is slightly wider than the average linecore width of ∼1 Å. If we interpret this excess width as due tomagnetic broadening, this would correspond to a field strengthon the order of 10 kG. The line core of WD1105-048 shows nopeculiarities, it has a normal width of 1 Å and thus no detectablefield.
HS 0051+1145. This object has previously been found as ablue source, PHL 886, but was not observed spectroscopicallybefore the SPY. It is a new magnetic DA. The SPY spectrahave a rather low S/N and thus only the Hα triplet of one ofthe spectra is resolved. The components are placed at 6558.9 Å,6563.6 Å, and 6568.6 Å, yielding an approximate field strengthof 240 ± 10 kG.
HE 1233−0519. This DA was published by Koester et al.(2001), but not recognized as a magnetic star. The SPY spec-tra have a low S/N such that only the Hα triplet is discernible inone of the spectra. With the components at 6552.2 Å, 6564.4 Å,and 6576.6 Å, a field strength of 610 ± 10 kG results.
WD 2051−208. Beers et al. (1992) published this object as aDA, but it was not further investigated since. It is a new mag-netic DA, and shows a variable Zeeman splitting of Hα andHβ. The Hα components in the two SPY spectra are found at6562.0 Å, 6566.6 Å, 6570.7 Å, and at 6560.2 Å, 6566.6 Å,6571.9 Å, respectively, and those of Hβ at 4861.2 Å, 4864.0 Å,4866.7 Å, and at 4861.0 Å, 4863.9 Å, 4866.9 Å. The resultingfield strengths are 220 ± 20 kG and 290 ± 20 kG (from Hα) aswell as 250 ± 30 kG and 270 ± 30 kG (from Hβ). The values de-rived from Hα are significantly different, and each is consistentwith the corresponding value from Hβ.
WD 2253−081 and WD 1344+106. Bergeron et al. (2001) sus-pected that shallow line cores which they found for theseobjects might indicate low-strength magnetic fields. The linecores of both objects have since been fitted with rotation-ally broadened line profiles, corresponding to projected rotationvelocities of 36+14
−7 km s−1 for WD 2253−081 (Karl et al. 2005)and 4.5 ± 2 km s−1 for WD 1344+106 (Berger et al. 2005). The
6540.0 6560.0 6580.0 6600.0
0.40
0.60
0.80
1.00
4700.0 4800.0 4900.0 5000.0
0.100
0.200
0.300
0.400
Δ λ [Α]
Fig. 5. Four new magnetic DAs. Top panel: Hα in WD2051-208, HS0051+1145, HE1223-0519 (from top). Bottom: Hβ inHS1031+0343. Vertical axis is relative intensity, with arbitrary offsetsbetween spectra for clarity.
Hα line cores in the SPY spectra of both objects neither showZeeman triplets nor flat bottoms that could indicate the presenceof a B field. They are non-magnetic objects.
HS0209+0832. This DAB star is well studied since it is oneof very few objects that exhibit helium features at a temperaturethat places it in the DB gap (Jordan et al. 1993). Heber et al.(1997) found a helium abundance that is variable at timescalesof a few months, which has been interpreted as a sign of he-lium accretion from a clumpy interstellar medium. The equiva-lent widths of the He i 4471 Å and 5876 Å lines show no signif-icant differences between both SPY spectra, i.e., no variation ofthe abundance is found. This is however not surprising since thespectra were recorded within 3 days of each other.
Zeeman splitted Hα or Hβ for the four new magnetic DAsare displayed in Fig. 5.
6. Binaries with DA white dwarfsand dM companions
Table 3 gives the data on binaries containing a DA and a M dwarfcompanion, identified from molecular features in the redspectrum and/or Balmer emission components. The names inboldface indicate new detections from the SPY. The magnitude
462 D. Koester et al.: High-resolution spectra observed for the SPY. III. DA white dwarfs
is the Johnson V magnitude, unless indicated otherwise (see de-scription for Table 1). The type is estimated from the effectivetemperature obtained with a fit with hydrogen models, usingonly the higher Balmer lines from Hγ.
7. Conclusions
We present the data – coordinates, magnitudes, and alias names –for the hydrogen-rich objects in the SPY sample. These in-clude 615 objects with pure hydrogen spectra, for which atmo-spheric parameters derived from fits with hydrogen models aregiven in Table 1. Of these, 187 are new white dwarf detectionsfrom this survey, or the HES and HQS surveys used to definethe target list. In addition to the 615 DAs, our sample also in-cludes 46 DA+dM binaries, of which 10 are new, and 10 mag-netic DA (4 new). The results show that with careful reductioneven high-resolution echelle spectra can be used to determinestellar parameters through line profile fitting, although the lineprofiles may extend over many echelle orders. However, thereis an indication that the surface gravities obtained are lowerby 0.05−0.08 dex, compared to results from high S/N low-resolution spectra. The surface gravities of the normal DAs showthe well known, but still unexplained, trend to a larger value (by0.2 dex) for temperatures below approximately 12 500 K.
Acknowledgements. T.L. is supported within the framework of the ExcellenceInitiative by the German Research Foundation (DFG) through the HeidelbergGraduate School of Fundamental Physics (grant number GSC 129/1). Researchat Bamberg in the context of the SPY project was funded by the DFG throughgrants Na 365/2-1/2 and He 1356/40-3/4. This research has made extensive useof the SIMBAD database, operated at CDS, Strasbourg, France.
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