ATA fluxes are lower than single-dish …pwilliam/williams_aas213...Exploring the FIR-Radio...
1
Rough timescales for escape from the galactic disk, synchrotron cooling (minimum-energy and equipartition field cases), and bremsstrahlung and ionization losses (“secondary processes”). Observed and predicted values of and d/d ln . The Thompson et al. values are computed from simple models with various physically-reasonable parameters. M82 M82 NGC 253 NGC 253 APG 220 APG 220 Calibrator cross-checks. Gaps in coverage are mostly due to lack of applicable observations, not RFI.
Transcript of ATA fluxes are lower than single-dish …pwilliam/williams_aas213...Exploring the FIR-Radio...
The
firs
t phas
e o
f th
e A
TA
was
fund
ed t
hro
ug
h
gen
ero
us
gra
nts
fr
om
the
Pau
l G
. A
llen
Fam
ily
Fo
und
atio
n.
UC
Ber
kel
ey,
the
SE
TI
Inst
itu
te,
the
Nat
ion
al
Sci
ence
F
ou
ndat
ion
(Gra
nt
No.
054
05
99
),
Sun
Mic
rosy
stem
s,
Xil
inx
, N
ath
an
Myh
rvo
ld,
Gre
g
Pap
ado
pou
los,
an
d
oth
er
corp
ora
tions
and
indiv
idu
al
dono
rs
contr
ibu
ted
addit
ional
fu
ndin
g.
PK
GW
was
fund
ed b
y a
n N
SF
G
rad
uat
e R
esea
rch
Fel
low
ship
.
Ex
plo
rin
g t
he
FIR
-Ra
dio
Co
rre
lati
on
wit
h C
on
tin
uo
us S
pe
ctr
a f
rom
th
e A
TA
Pe
ter
K.
G.
Wil
lia
ms
UC
Be
rkele
Ge
off
rey
C.
Bo
we
rU
C B
erk
ele
All
of
the
soft
war
e u
sed
in t
he
exec
uti
on o
f th
is p
roje
ct i
s F
ree
or
open
sou
rce.
Th
is w
ould
not
be
po
ssib
le w
ith
ou
t th
e ti
rele
ss
effo
rt o
f co
ntr
ibuto
rs t
o a
vas
t ar
ray
of
pro
ject
s, i
ncl
ud
ing
:
Th
e L
inux
ker
nel
T
he
GN
U P
roje
ct
Th
e P
yth
on l
angu
age
��
IPy
thon
Num
eric
al a
nd
Sci
enti
fic
Pyth
on
MIR
IAD
��
Th
e G
NO
ME
Des
kto
p
Cai
ro
Open
Off
ice.
org
O
meg
aPlo
t�
��
git
T
he
GN
U I
mag
e M
anip
ula
tion P
rogra
m�
Rec
ent
theo
reti
cal
work
advoca
tes
the
"cal
ori
met
er"
inte
rpre
tati
on o
f th
e F
IR-r
adio
corr
elat
ion.
Publi
shed
dat
a an
d n
ew c
onti
nuous
spec
tra
from
the
All
en T
eles
cop
e A
rray
len
d s
up
port
to t
he
theo
ry.
Ba
ck
gro
un
dT
he
corr
elat
ion
bet
wee
n
the
far-
infr
ared
(F
IR)
and
rad
io
emis
sion
of
no
rmal
gal
axie
s is
st
rik
ing
fo
r it
s ti
gh
tnes
s a
nd
th
e ra
ng
e of
con
dit
ion
s in
w
hic
h it
h
old
s. B
road
ly sp
eakin
g,
emis
sion
in
b
oth
ban
ds
trac
es
rece
nt
star
form
atio
n (
SF
). B
ut
the
det
ails
are
u
ncl
ear:
h
ow
is
li
nea
rity
m
ain
tain
edo
ver
such
a w
ide
range
of
cond
itio
ns?
Th
e "
calo
rim
eter
"
mod
el o
f V
ölk
(1
989
) posi
ts
that
co
rrel
atio
n
hold
s b
ecau
se
radio
-em
itti
ng
elec
tron
s co
ol
com
ple
tely
w
ithin
a
smal
l volu
me.
T
hom
pso
n
et
al.
(2006)
suppo
rt
the
mod
el,
arg
uin
g t
hat
sta
rbu
rst
gala
xie
s h
av
e m
uch
str
on
ger
magn
etic
fie
lds
tha
n co
mm
on
ly a
ssu
med
, le
adin
g to
ra
pid
sy
nch
rotr
on c
ooli
ng (
bel
ow
).
To re
bu
t a
co
mm
on cr
itic
ism
�
that
o
bse
rved
ga
lact
ic
spec
tra
are
to
o
sha
llo
w t
o b
e sy
nch
rotr
on
-coole
d �
Th
om
pso
n et
a
l. c
onsi
der
io
niz
ati
on
a
nd
b
rem
sstr
ah
lun
g
loss
es,
whic
h
ten
d
to
flat
ten
spec
tra.
T
hei
r m
odel
s p
red
ict
dev
iati
on
s fr
om
pu
re p
ow
er
law
s i
n
ob
serv
ed
nonth
erm
al
spec
tra.
T
he
AT
A (
Wel
ch e
t al.
2009
) i
s w
ell-
suit
ed t
o t
esti
ng
th
ese
pre
dic
tio
ns.
AT
A O
bse
rvati
on
s a
nd
Da
ta R
ed
uc
tio
n� M
82, A
PG
220, an
d N
GC
253 w
ere
obse
rved
for
9 h
ou
rs o
ver
6 e
poch
s in
~
1-m
inute
snap
sho
ts, w
ith c
alib
rato
rs
3C
48,
3C
147, an
d 3
C 2
86
� F
requen
cies
ran
ged
fro
m 0
.5 G
Hz
to
7 G
Hz,
skip
pin
g b
ands
wit
h s
ever
e R
FI,
wit
h a
ban
dw
idth
of
100 M
Hz
� F
lux
cal
ibra
tion w
as r
elat
ive
to V
LA
1999.2
model
s, w
hic
h g
ave
the
most
se
lf-c
onsi
sten
t re
sult
s
� C
ross
-chec
ks
com
par
ing c
alib
rato
r obse
rvat
ions
to m
odel
s (b
elow
) sh
ow
th
e pip
elin
e w
ork
s w
ell
� I
ndiv
idual
sca
ns
wer
e pro
cess
ed
separ
atel
y s
o t
hat
rep
eata
bil
ity c
ould
be
asse
ssed
� R
eport
ed v
alues
are
the
wei
ghte
d
aver
age
of
one
or
more
sca
ns
� O
bse
rvat
ions
by t
he
AT
A h
ad a
ty
pic
al
snap
shot
flu
x p
reci
sion
of
5%
(ri
ght)
var
yin
g w
ith s
ourc
e fl
ux
� R
esult
s ar
e se
par
ated
by
cal
ibra
tor
so
model
inac
cura
cies
can
be
iden
tifi
ed
Re
fere
nces
[A+
00]
Anan
thara
mai
ah, K
. R
., V
iall
efo
nd,
F., M
ohan, N
. R
.,
Goss
, W
. M
., &
Zhao, J.
-H.
2000, A
pJ,
537
, 61
3[B
+79]
Bec
k, R
., B
ierm
ann, P
., E
mer
son, D
. T
., &
W
iele
bin
ski,
R. 197
9, A
&A
, 7
7, 25
[CK
91
] C
arls
trom
, J.
E.
& K
ronb
erg, P
. P
. 1991, A
pJ,
366, 422
Condon, J.
J., C
ott
on, W
. D
., G
reis
en, E
. W
., Y
in, Q
. F
.,
Per
ley, R
. A
., T
aylo
r, G
. B
., &
Bro
der
ick,
J. J
. 199
8, A
J,
115, 1693
Condon, J.
J., A
nder
son, M
. L
., &
Hel
ou
, G
. 1991, A
pJ,
376,
95
This
w
ork
h
as m
ade
use
o
f th
e N
RA
O V
LA
S
ky
Su
rvey
(C
ond
on
et
al.
, 1998
).
This
re
sear
ch
has
m
ade
use
of
the
NA
SA
/IP
AC
Ex
trag
alac
tic
Dat
abas
e (N
ED
) w
hic
h
is
oper
ated
b
y
the
Jet
Pro
pu
lsio
n
Lab
ora
tory
, C
alif
orn
ia
Inst
itute
of
Tec
hnolo
gy
, u
nd
er
contr
act
wit
h
the
Nat
ional
A
eronau
tics
an
d
Spac
e A
dm
inis
trat
ion.
This
res
earc
h h
as m
ade
use
of
the
SIM
BA
D d
atab
ase,
oper
ated
at
CD
S,
Str
asb
ou
rg,
Fra
nce
.
Ro
ugh
tim
esca
les
for
esca
pe
from
the
gal
acti
c dis
k,
syn
chro
tro
n c
oo
ling
(min
imu
m-e
ner
gy
and
equ
ipar
titi
on f
ield
case
s),
and
bre
mss
trah
lung
and
ion
izat
ion l
oss
es
(“se
con
dar
y
pro
cess
es”)
.
Dow
nes
, D
. &
Solo
mon, P
. M
. 1999, A
pJ,
507
, 61
5[G
W8
1]
Gel
dzah
ler,
B. J.
& W
itze
l, A
. 198
1, A
J, 8
6, 1306
Gib
son, J.
, W
elch, W
. J.
, &
de
Pate
r, I
. 2005, Ic
aru
s, 1
73, 439
[K+
88]
Kle
in, U
., W
iele
bin
ski,
R.,
& M
ors
i, H
. W
. 1988,
A&
A,
190, 41
Macq
uart
, J.
-P.
& d
e B
ruy
n, A
. G
. 2007, M
NR
AS
, 380, L
20
[Par
kes
90]
Par
kes
Cata
log
ue, 19
90,
Aust
rali
a T
eles
cope
Nat
ion
al F
aci
lity
O'D
ea, C
. P
., B
aum
, S
. A
., S
tanghel
lini,
C.,
Morr
is, G
. B
.,
Pat
nai
k,
A.
R., &
Go
pal
-Kri
shna. 1990, A
&A
S, 84, 549
Rea
dhea
d,
A. C
. S
., T
aylo
r, G
. B
., X
u, W
., P
ears
on,
T. J.
, W
ilkin
son
, P
. N
., &
Pola
tidis
, A
. G
. 1996, A
pJ,
460, 612
[R+
06]
Ric
ci,
R., P
randoni,
I., G
rup
pio
ni,
C., S
ault
, R
. J.
, &
de
Zott
i, G
. 2
006
, A
&A
, 445, 465
[R+
05]
Rodrí
guez-
Ric
o, C
. A
., G
oss
, W
. M
., V
iall
efon
d, F
.,
Zhao,
J.-H
., G
óm
ez, Y
., &
Anan
thara
maia
h, K
. R
. 2005,
Ap
J, 6
33, 198
[SA
91]
Sopp
, H
. M
. &
Ale
xander
, P
. 1991, M
NR
AS
, 251, 112
[S+
04]
Str
ickla
nd, D
. K
., H
eck
man
, T
. M
., C
olb
ert,
E. J.
M.,
Hoopes
, C
. G
., &
Wea
ver
, K
. A
. 20
04,
Ap
J, 6
06, 829
Tho
mp
son, T
. A
., Q
uat
aer
t, E
., W
axm
an, E
., M
urr
ay, N
., &
M
arti
n, C
. L
. 2
006
, A
pJ,
645
, 18
6V
ölk
, H
. J.
19
89,
A&
A,
218
, 67
Wel
ch, W
. J.
, and 4
3 c
oauth
ors
. 2009, P
roc.
IE
EE
, su
bm
itte
d
� M
odel
s o
f th
erm
al a
nd
non
ther
mal
contr
ibu
tion
s w
ere
fit
to t
he
ob
serv
ed s
pec
tra
and
dat
a fr
om
the
lite
ratu
re.
� T
he
fits
to A
TA
dat
a w
ere
augm
ente
d w
ith
hig
h-f
requ
ency
p
oin
ts f
rom
the
lite
ratu
re t
o
bet
ter
con
stra
in t
he
ther
mal
fr
acti
on
. F
or
M82, th
e 32 G
Hz
poin
t w
as s
cale
d b
y 8
6%
.
� A
TA
flu
xes
are
low
er t
han
si
ngle
-dis
h m
easu
rem
ents
, p
oss
ibly
due
to e
xte
nded
em
issi
on b
eing r
eso
lved
out
on
angu
lar
scal
es o
f te
ns
of
arcm
in.
AT
A a
nd V
LA
mea
sure
men
ts
agre
e w
ell.
� T
he
AT
A d
ata
are
pre
sen
ted
above
N
ote
s: S
ee S
pec
tra
l M
odel
ing
for
det
ails
on t
he
model
s.
Unce
rtai
nti
es
com
e fr
om
th
e sc
atte
r in
re
pea
ted
mea
sure
men
ts.
For
com
par
ison
, th
e M
82
plo
t sh
ow
s in
div
idual
sc
ans,
n
ot
wei
gh
ted av
erag
es.
NG
C 253 w
as
reso
lved
in
to a
poin
t-so
urc
e co
re a
nd a
n e
llip
tica
l ex
tended
co
mpon
ent;
sep
arat
e an
d t
ota
l fl
uxes
are
sh
ow
n.
Sp
ec
tra
l M
od
elin
g
Fu
ture
Dir
ecti
on
s. O
ther
use
s fo
r co
nti
nuous
spec
tra
incl
ud
e: [
1]
Obta
inin
g a
ccura
te a
ges
and
lum
inosi
ties
of
gig
aher
tz
pea
ked
-spec
trum
(G
PS
) so
urc
es
(e.g
.O
'Dea
et
al.
1990)
and
com
pac
t sy
mm
etri
c obje
cts
(CS
Os)
(e
.g.
Rea
dhea
d
et
al.
1996).
[2
] F
ull
y
char
acte
rizi
ng
scin
till
atio
n
pro
cess
es
of
intr
aday
var
iab
les
(ID
Vs)
(e.
g.
Mac
quar
t &
de
Bru
yn 2
007).
[3
] P
robin
g
atm
osp
her
ic
chem
istr
y
of
Jupit
er
and
Sat
urn
(e.
g. G
ibso
n e
t a
l. 2
005
)
Les
son
s L
earn
ed.
Ex
per
ience
s re
levan
t to
E
VL
A
and S
KA
: [1
] A
ccura
te b
road
ban
d c
alib
rato
r m
od
els
are
lack
ing;
var
iabil
ity
is
an
is
sue
at
hig
her
fr
equen
cies
. [2
] E
xis
ting v
isual
izat
ion an
d an
aly
sis
tools
hav
e tr
oub
le c
opin
g w
ith m
any a
nte
nnas
and
spec
tral
ch
annel
s.
New
so
ftw
are
is
nec
essa
ry t
o
mak
e th
e m
ost
of
new
har
dw
are.
Resu
lts a
nd
Co
nc
lusio
ns
Ther
e is
su
gges
tive
evid
ence
th
at
the
ma
gn
etic
fie
ld B
> B
min
in t
he
obse
rved
gal
axie
s, l
end
ing s
up
port
to
the
calo
rim
eter
mod
el.
� T
he
non
ther
ma
l sp
ectr
a s
teep
en i
n
the
GH
z re
gim
e, a
s p
red
icte
d i
n
Th
om
pso
n e
t al.
, al
though t
his
can
be
expla
ined
in B
= B
min
model
s.
� O
bse
rved
sp
ectr
al
ind
exes
at
5 G
Hz
are
con
sist
ent
wit
h p
red
icti
on
s m
ade
by T
hom
pso
n e
t al.
Ther
e is
si
gnif
ican
t dis
agre
emen
t at
1 G
Hz,
w
her
e fr
ee-f
ree
abso
rpti
on m
ay
bec
om
e a
fact
or.
�T
he
ob
serv
ed s
pec
tra
ste
epen
mo
re
than
pre
dic
ted
(ri
ght)
. S
olv
ing t
his
dis
crep
ancy
wil
l be
an
im
port
an
t te
st f
or
the
Th
om
pso
n e
t al.
mod
el.
Ob
serv
ed a
nd
pre
dic
ted
val
ues
of �
and
d�
/d l
n �
. T
he
Th
om
pso
n e
t a
l.
val
ues
are
com
pu
ted
fro
m s
imp
le m
odel
s
wit
h v
ario
us
physi
call
y-r
easo
nab
le
par
amet
ers.
� T
he
bes
t-fi
t m
od
els
are
sh
ow
n a
t ri
gh
t. T
he
dat
a fr
om
th
e li
tera
ture
com
e fr
om
a
var
iety
of
inst
rum
ents
. T
he
AP
G 2
20 A
TA
dat
a w
ere
too
n
ois
y t
o y
ield
use
ful
fits
.
� T
he
form
al
erro
rs a
re ~
10%
, b
ut
thes
e ar
e u
nder
esti
mat
es
du
e to
eff
ects
lik
e po
inti
ng
erro
rs a
nd p
has
e sc
atte
r.
M82
M82
NG
C253
NG
C253
AP
G220
AP
G220
Cal
ibra
tor
cross
-chec
ks.
Gap
s in
cover
age
are
most
ly d
ue
to
lack
of
appli
cab
le
obse
rvat
ion
s,
not
RF
I.
