Measuring the properties of QSO broad- line regions with the GMOS IFU. Randall Wayth with Matt...
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Transcript of Measuring the properties of QSO broad- line regions with the GMOS IFU. Randall Wayth with Matt...
Measuring the properties of QSO broad-line regions with the GMOS IFU.
Randall Waythwith Matt O'Dowd & Rachel Webster.
Outline
Motivation Introduction to 2237+0305 Observations & Data reduction Emission line flux ratios Microlensing of QSO emission regions Constraints on emitting region size
Motivation - QSO emission regions QSO continuum/line emission regions are too
small to resolve Reverberation mapping suggests they are very
small Gravitational lensing magnifies objects. If a
source is resolved in a lensed image, then we can directly determine its true size & surface brightness
If not resolved, then microlensing should create different magnifications for the continuum and broad-line regions of the QSO.
2237+0305
Barred spiral (Sbc) galaxy at low redshift (z=0.04) lensing z=1.69 radio quiet QSO.
Four images of QSO formed around galaxy bulge with separation ~1-2 arcsec
Lensing offers unique opportunity to study
• QSO continuum and emission line region size/structure
• Properties of dark matter halo (shape, cuspiness, clumpiness)
• Mass function of galaxy bulge stars, and more...
Is the CIII] emission region in 2237+0305 resolved?
Mediavilla et al. (1998) claimed seeing an arc of resolved CIII] emission using INTEGRAL IFU on WHT. (0.5” separation, rectangular array, 0.45” fibre diameter)
If real, we can “undo” the effects of lensing and create a true image of the emission region.
From Mediavilla et al. (1998) ApJ 503 L27
Data - GMOS IFU
IFU is a hexagonal lenslet array with separation 0.2”
R400 grating in “one slit” mode. Useful wavelength range ~500-850nm. Object coverage is 5”x3”.
8 x 30min exposures taken on 16/17 July, 2002. We use 5 of the 8 frames. Seeing 0.6”
ObjectSky
Aims
Confirm/refute existence of arc of emission If real, make an image of the QSO BELR! If not real, examine effect of lensing on the
relative strengths of continuum and broad-line emission from the QSO
Images of the broad-line flux Subtracting surrounding continuum from the
emission lines leaves the line flux Subtraction is quite clean Notice difference in brightness of QSO images
CIII] continuum CIII] - emission lineMgII continuum MgII – emission line
Arc or PSF overlap?
PSF modelling & subtraction We are looking for a faint arc, so we need to
create an accurate PSF and subtract the QSO images.
Method
• combine line images for the 5 good frames
• define a mask around each QSO image including a region which is uncontaminated by other images
• cut out, rescale and combine sections from each image
• use this PSF, to subtract QSO images, iterate a few times
Line images with QSOs subtracted
Unresolved! - No arc in MgII or CIII]! Peak residual ~10%
MgIICIII]
Microlensing and the BELR Microlensing by stars in
the lens galaxy's bulge project a network of “caustics” onto the QSO.
Parts of the source crossing caustics (red/yellow) are highly magnified.
The QSO can be differentially magnified depending on its size relative to the caustic network.
Microlensing caustic networkImage courtesy Joachim Wambsganss
Microlensing and the BELR Small source = no
differential magnification
All parts of the source are equally magnified
Microlensing and the BELR Medium source =
differential magnification!
If the QSO's continuum region is much smaller than the BELR, then the continuum should be more highly magnified.
Flux ratios
A
DB
C
Galaxy centre
Extinction corrected flux ratios for continuum and broad-lines are certainly different!
Without microlensing, all images should have approx same magnitude, so BELR is also microlensed.
Because MgII and CIII] lines have same flux ratio, they must be similar size.
BELR size ~0.06pc based on simulations of Wyithe et. al 2002 (MNRAS 331)
Next: de-dispersed spectral ratios
After correcting for atmospheric dispersion, take ratios of image spectra
Broad-line magnifications clearly visible
Shape of continuum is a function of source morphology, microlensing and extinction
Shape/location of lines depends on BELR structure!
C/A
D/A
B/A
5000 6000 7000 8000
Summary
Using GMOS-N IFU we have taken the best spectroscopic data of 2237+0305 to date
We find no arc of emission in either the CIII] or MgII line, contrary to previous claims
Magnification ratios of the images in both the continuum and broad-lines show microlensing
BELR is measured from flux ratios to be ~0.06pc. This estimate will improve using de-dispersed data.
MNRAS 359 561 (2005)