Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.arcetri.astro.it/igm50/talks_all/straka.pdf Äàòà èçìåíåíèÿ: Wed Jun 17 11:43:54 2015 Äàòà èíäåêñèðîâàíèÿ: Sun Apr 10 02:08:31 2016 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: arp 220

Galactic Nebular Emission in QSO Spectra
Lorrie Straka
P. Noterdaeme (IAP), D. York (UC), R. Srianand (IUCAA), D. Bowen (Princeton), V. Kulkarni (USC), M. Subbarao (Adler), G. Richards (Drexel), D. Vanden Berk (SVC), P. Hall (York), T. Heckman (JHU), P. Khare (IUCAA), J. Quashnock (UC), M. Bishof (UC), Z. Wichard (NWU), S. Kuttruff (Carthage), L. Ghering (UC), S. Johnson (UC), S. Nutalaya (UC)

June 2015
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Tuesday, June 9, 15


Outline
· · · ·
What are Galaxies on Top of QSOs (GOTOQs)? Searching for GOTOQS Proper ties of GOTOQs The future: utilizing MUSE in absorption line studies

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Tuesday, June 9, 15


What are GOTOQs?
· · ·
Low-z quasar-galaxy pair s found in the SDSS Some or all of the galaxy falls within the 3 arcsecond spectral fiber centered on the quasar Q1042+0748 (Bor thakur et al. 2010)

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Tuesday, June 9, 15


Searching for GOTOQs
· · ·
QSO spectra have over lapping narrow emission lines indicating the presence of inter vening galaxies within 1.5" >100,000 QSO spectra searched Sample of 103 late-type galaxies

·

Full photometric and spectroscopic set of measurements

Galactic emission lines: [OII], Hb, [OIII],[NII], Ha, [SII]
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Tuesday, June 9, 15


Searching for GOTOQs
·
QSO spectra have over lapping narrow emission lines indicating the presence of inter vening galaxies within 1.5"

z(em)=0.046

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Tuesday, June 9, 15


Role rever sal: compile a catalog of low-z GOTOQs detected in emission, and then search for absorption

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Tuesday, June 9, 15


Questions to Address
· · · · ·
What are the environments along quasar lines of sight? What are the roles of outflows and inflows? Photometric and spectroscopic proper ties How are emission and absorption proper ties connected? How are low-z absorption systems related to higher-z absorption systems?

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Tuesday, June 9, 15


Questions to Address
· · · · ·
What are the environments along quasar lines of sight?

·

Effect of groups or isolation, IGM

What are the roles of outflows and inflows? Photometric and spectroscopic proper ties How are emission and absorption proper ties connected? How are low-z absorption systems related to higher-z absorption systems?

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Tuesday, June 9, 15


Questions to Address
· · · · ·
What are the environments along quasar lines of sight? What are the roles of outflows and inflows?

·

Orientation and inclination angle

Photometric and spectroscopic proper ties How are emission and absorption proper ties connected? How are low-z absorption systems related to higher-z absorption systems?

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Tuesday, June 9, 15


Questions to Address
· · · · ·
What are the environments along quasar lines of sight? What are the roles of outflows and inflows? Photometric and spectroscopic proper ties

·

Morphology, luminosity, SFR, metallicity

How are emission and absorption proper ties connected? How are low-z absorption systems related to higher-z absorption systems?

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Tuesday, June 9, 15


Questions to Address
· · · · ·
What are the environments along quasar lines of sight? What are the roles of outflows and inflows? Photometric and spectroscopic proper ties How are emission and absorption proper ties connected? How are low-z absorption systems related to higher-z absorption systems?

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Tuesday, June 9, 15


Questions to Address
· · · · ·
What are the environments along quasar lines of sight? What are the roles of outflows and inflows? Photometric and spectroscopic proper ties How are emission and absorption proper ties connected? How are low-z absorption systems related to higher-z absorption systems?

·
Tuesday, June 9, 15

Evolutionar y processes

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Why GOTOQs?
· · ·
Low-z galaxies are more easily detectable in emission (spectroscopically and in imaging!) At low redshifts, the strongest obser vable absorption features are Ca II and Na I Mg II, Mg I, and Fe II are other strong features to seek at z>0.4

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Tuesday, June 9, 15


Results
· · · · ·
58 of 103 GOTOQs have visible galaxy and absorption 10 with no visible galaxy and no Ca II or Na I absorption at z<0.4 All impact parameter s < 12 kpc Low luminosities : ~50% of the sample have L* values in the dwarf range (L*<0.2) Typical SFR < 5 Msol yr
-1

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Tuesday, June 9, 15


Results
· · · ·
58 of 103 GOTOQs have visible galaxy and absorption 10 with no visible galaxy and no Ca II or Na I absorption at z<0.4 All impact parameter s < 12 kpc Typical SFR < 5 Msol yr
-1

·

Low luminosities : ~50% of the sample have L* values in the dwarf range (L*<0.2)

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Tuesday, June 9, 15


Results
· · · · ·
Tuesday, June 9, 15

58 of 103 GOTOQs have visible galaxy and absorption 10 with no visible galaxy and no Ca II or Na I absorption at z<0.4 Low luminosities : ~50% of the sample have L* values in the dwarf range (L*<0.2) All impact parameter s < 12 kpc Typical SFR < 5 Msol yr
-1

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Results
· ·
Stellar mass estimates via HyperZ cover a wide range Imaging non-detections due to low surface brightness

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Tuesday, June 9, 15


Results

Ca II EW and Ha flux: Ca II traces dusty environments! H-alpha direct indicator of SF
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Tuesday, June 9, 15

Ca II EW and [O III] flux: [O III] dependent on ne ,Te; indirect indicator of SF


Results
Color excess vs. impact parameter : Higher dust content near the center s of galaxies. Color excess vs. galaxy color : Dustier systems are systematically more red (no surprise)

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Tuesday, June 9, 15


Resulting Publications
· · · · · ·
Bor thakur et al. 2010 Noterdaeme et al. 2010 Yor k et al. 2012 Srianand et al. 2013 Straka et al. 2013 Straka et al. 2015

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Tuesday, June 9, 15


Resulting Publications
· · · · · ·
Bor thakur et al. 2010 Noterdaeme et al. 2010 Yor k et al. 2012 Srianand et al. 2013 Straka et al. 2013 Straka et al. 2015

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Tuesday, June 9, 15


Summar y
· · · · ·
Tuesday, June 9, 15

GOTOQs selected by emission are primarily isolated latetype galaxies with low SFR High reddening indicating the presence of dust Correlations between b, (u-r) and E(B-V) and H-alpha, [O III]
(g-i);

Ca II EW

No correlations between Ca II EW and b, E(B-V)

(g-i)

Future wor k: refer to the list of questions! (+HST)

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