Understanding Post-Starburst Quasars and Their Role in Mutual Black Hole - Bulge

Growth in Galaxies

Understanding Post-Starburst Quasars and Their Role in Mutual Black Hole - Bulge

Growth in Galaxies

A Thesis Proposal by:Sabrina L. Cales

This 20th of February, 2008

A Thesis Proposal by:Sabrina L. Cales

This 20th of February, 2008

MBH ~ 0.15% Mbulge => M-*

MBH ~ 0.15% Mbulge => M-*

Gebhardt et al. 2000

The Antennae Galaxieshttp://antwrp.gsfc.nasa.gov/apod/ap971022.html

http://astronomy.swin.edu.au/cosmos/H/Hierarchical+Merging

Hierarchical MergingHierarchical Merging Toomre (1977) Toomre (1977)

Di Matteo, Springel & Hernquist 2005

Simulation

Di Matteo, Springel & Hernquist 2005

Simulation

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Di Matteo, Springel & Hernquist 2005

Di Matteo, Springel & Hernquist 2005

Di Matteo, Springel & Hernquist 2005

Di Matteo, Springel & Hernquist 2005

• Mergers induce inflows which feed the quasar• Feedback from quasar and SN extinguishes further BH growth and star formation• Crucial impact on the evolution of the galaxy

• Mergers induce inflows which feed the quasar• Feedback from quasar and SN extinguishes further BH growth and star formation• Crucial impact on the evolution of the galaxy

The Importance of Being UltraluminousThe Importance of Being Ultraluminous

ULIRGshttp://www.utahskies.org/report/20021018/20021018weekly.html

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Quasar HostsBennert et al. 2008

Quasar HostCanalizo et al. 2007

• ULIRGs predominantly merging systems• Quasar hosts are disturbed and interacting!• ULIRGs predominantly merging systems• Quasar hosts are disturbed and interacting!

Evolutionary SchemaEvolutionary Schema

Hopkins et al. 2007, this is a ‘doctored’ version

?

Begin here…

…over time begins to group

Increase in star formation

Coalescence, gas inflow to center (starburst and buried AGN)

Rapid BH growth, expelling of dust & gas, high L/Ledd,

visible merger signatures

‘Traditional’, fading of tidal

features

Starburst remnant from ULIRG phase,

rapid reddening, some tidal features

No star formation, large black hole/bulge

PSQs and Prototype UN J1025-0040

PSQs and Prototype UN J1025-0040

+ =

• PSQs are composite objects• Quasar plus A-type population spectra• UN J1025-0040:

-Companion galaxy in post-SB phase-~400 Myr old SB-Host merger remnant

• PSQs are composite objects• Quasar plus A-type population spectra• UN J1025-0040:

-Companion galaxy in post-SB phase-~400 Myr old SB-Host merger remnant

Brotherton et al. 2001

Brotherton et al. 1999

Brotherton et al. 1999

Valdes et al. 2004109 solar masses100s of Myr

PSQSDSS J074621.06+335040.7

Brotherton et al. 2008b, in preparation

~600 PSQs from SDSS DR3Brotherton et al. 2008a, in prepSpectroscopically selected from

quasar catalog, H

Large-scale, 10-100 kpc• PSQs have more neighbors than quasars - 4:3• More PSQs have neighbors than quasars - 90%:76%

Small-scale, <10 kpc• Binned 10% by size-scale• Stacked images • Host galaxies have different

shapes• Host galaxy contributes more

in the PSQs than quasar

~600 PSQs from SDSS DR3Brotherton et al. 2008a, in prepSpectroscopically selected from

quasar catalog, H

Large-scale, 10-100 kpc• PSQs have more neighbors than quasars - 4:3• More PSQs have neighbors than quasars - 90%:76%

Small-scale, <10 kpc• Binned 10% by size-scale• Stacked images • Host galaxies have different

shapes• Host galaxy contributes more

in the PSQs than quasar

PSQ Catalog and Environments

PSQ Catalog and Environments

Project DescriptionProject Description

Determine the properties and nature of PSQs Imaging of HST SampleHost and quasar component analysis Infrared Properties of PSQsPopulation analysis and comparison/constraining of

theoretical models

Determine the properties and nature of PSQs Imaging of HST SampleHost and quasar component analysis Infrared Properties of PSQsPopulation analysis and comparison/constraining of

theoretical models

Imaging Spectroscopy

HST, F606W (R)

IRTF, K-band Keck/KPNO,

opticalSpitzer,

mid-infrared

Number of PSQs

29 29 28 16

HST ImagingHST Imaging

HST Sample: 29 ACS SNAPshot F606W images from target list of 80, r < 18.6, H EW >1A, 0.25 < z < 0.45

MorphologiesQuasar to host light

…contributions to …constrain EPS

IRTF K-band Data and Analysis

HST Sample: 29 ACS SNAPshot F606W images from target list of 80, r < 18.6, H EW >1A, 0.25 < z < 0.45

MorphologiesQuasar to host light

…contributions to …constrain EPS

IRTF K-band Data and Analysis Cales 2008, Thesis Proposal

Keck/KPNO SpectroscopyKeck/KPNO

Spectroscopy Keck LRIS, 3100Å-1m, 2 nights, observers - M. Brotherton

& G. Canalizo, reductions - G. Canalizo & S. Cales KPNO-4m RC-Spec, 3200Å-7200Å, 4 nights, observers - Z.

Shang & S. Cales, reductions - S. Cales

Keck LRIS, 3100Å-1m, 2 nights, observers - M. Brotherton & G. Canalizo, reductions - G. Canalizo & S. Cales

KPNO-4m RC-Spec, 3200Å-7200Å, 4 nights, observers - Z. Shang & S. Cales, reductions - S. Cales

Cales 2008, Thesis Proposal

Courtesy of R. Ganguly

Evolutionary Stellar Population Synthesis

(EPS)

Evolutionary Stellar Population Synthesis

(EPS) Compute spectral

evolution of stellar populations

Input model parameters: age, metallicity, star formation histories, dust content

Constrained by quasar to host light contribution from HST and IRTF imaging

Sought parameters: mass and starburst age

Compute spectral evolution of stellar populations

Input model parameters: age, metallicity, star formation histories, dust content

Constrained by quasar to host light contribution from HST and IRTF imaging

Sought parameters: mass and starburst age

Stars from Horizons: Seeds

Z=0.02, solar

EPS Models, Bruzual & Charlot 2001

Brotherton et al. 2001

Quasar Component Analysis

Quasar Component Analysis

Black hole mass via virial estimates, MBH~RV2/G using L as a proxy for R

Absorption of Balmer lines, use MgII

Eddington luminosity fractions, L/LEdd

Black hole mass via virial estimates, MBH~RV2/G using L as a proxy for R

Absorption of Balmer lines, use MgII

Eddington luminosity fractions, L/LEdd

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Brotherton et al. 2001

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IR PropertiesIR Properties

Spitzer IRS, low resolution, 5-40m, reductions - S. Cales

Spitzer IRS, low resolution, 5-40m, reductions - S. Cales

f(25m)/f(60m)<0,‘cool’

f(25m)/f(60m)>0,‘warm’

What do you get when you cross a quasar with a post-starburst population in the IR?

Color diagnostic, mid-IR slope Forbidden line - PAH EW

diagnostic

What do you get when you cross a quasar with a post-starburst population in the IR?

Color diagnostic, mid-IR slope Forbidden line - PAH EW

diagnostic

Dale et al. 2006, the above is ‘doctored’

How do PSQs fit in the Grand

Scheme of Things?

How do PSQs fit in the Grand

Scheme of Things?

How do other classes compare to the characteristic properties of PSQs? Is this in accord with the hypothesis? Morphologies Starburst ages &

Quasar/Host light contribution

Black Hole demographics-MBH, L/Ledd

IR Shape PAH features SB/Host light contribution

How do other classes compare to the characteristic properties of PSQs? Is this in accord with the hypothesis? Morphologies Starburst ages &

Quasar/Host light contribution

Black Hole demographics-MBH, L/Ledd

IR Shape PAH features SB/Host light contribution

Class Reference Study

ULIRGs

Netzer et al. (2007)Schweitzer et al. (2006)

QUEST: SED, colorsQUEST: Forbidden diagnostic lines and PAH emission

Quasars

Bennert et al. (2008) & Canalizo et al. (2007) Lacy et al. (2002)

Hosts: SB age, morphology and % contributionHosts: Morphology, % contribution, MBH, L/LEdd

Post-Starburst Galaxies

Goto et al. (2006)

Norton et al. (2001)

2D Spectra: Morphology, % contribution, colorsSpectra: Morphology, *, age

How do PSQs fit in the Grand

Scheme of Modeling?

How do PSQs fit in the Grand

Scheme of Modeling?

Models make specific predictions as to: L/Ledd, MBH, Mbulge, Colors, SB age, % contributions

Can we put classes on a time sequence?

Constrain models

Models make specific predictions as to: L/Ledd, MBH, Mbulge, Colors, SB age, % contributions

Can we put classes on a time sequence?

Constrain models

ULIRG

PSQ

PS Gal

quasar

elliptical

spiralcoalescence

Di Matteo, Springel & Hernquist 2005

OverviewOverview

M-* Hierarchical Merger ‘Blowout’

PSQs

Optical SpectraImaging Grand SchemeIR Spectra

TimelineTimeline Winter 2008 - Candidacy Exam, HST and IRTF Imaging and PSF subtraction, Begin Paper I

(Imaging of HST Sample), Begin Dissertation (Chapters 1 and 2) Spring 2008 - Continue with HST data analysis (AGN to host galaxy light fraction), Complete and

Submit Paper I to Astrophysical Journal, Continue with Dissertation (Complete Chapters 1 and 2) Summer 2008 - Reduce Kitt Peak 4-m data, Recalibrate Keck data, EPS of optical data constrained

by AGN to host galaxy light fraction, Chandra proposal (Other), Begin Paper II (EPS of optical data), Continue with Dissertation (Chapter 3)

Fall 2008 - Travel?: Porto Alegre, Brazil (M. Brotherton, Collaboration), Riverside, CA (G. Canalizo, EPS Tutorial), Finish analysis (AGN and starburst demographics) for and writing Paper II (Submit to ApJ), Prepare results for AAS meeting, Continue with Dissertation (Complete Chapter 3)

Winter 2009 - Present results at Long Beach, CA AAS meeting, Reduce Spitzer data, IR diagnostics (Color and PAH features), Begin Paper III (IR diagnostics), Continue with Dissertation (Chapter 4)

Spring 2009 - Finish IR diagnostics analysis (Color and PAH features), Complete Paper III (Submit to ApJ), Continue with Dissertation (Complete Chapter 4), Travel? China (Z. Shang, Collaboration

Summer 2009 - Collect data of other classes of objects and modeling, Herschel proposal (Other), Begin writing Paper IV (Comparisons of PSQs with objects and models), Teach a summer Astronomy 1050 Course, Continue with Dissertation (Chapters 5 and Other)

Fall 2009 - Finish analysis for and writing Paper IV, Job search and applications, Continue with Dissertation (Complete Chapter 5), Begin final analysis

Winter 2010 - Wrap up ‘Other’ if necessary, Job search and applications, Continue with Dissertation (Complete Final Chapters), Prepare for Dissertation Defense and AAS Meeting

Spring 2010 - Defend Dissertation and present at AAS Meeting, Get a Job!

Winter 2008 - Candidacy Exam, HST and IRTF Imaging and PSF subtraction, Begin Paper I (Imaging of HST Sample), Begin Dissertation (Chapters 1 and 2)

Spring 2008 - Continue with HST data analysis (AGN to host galaxy light fraction), Complete and Submit Paper I to Astrophysical Journal, Continue with Dissertation (Complete Chapters 1 and 2)

Summer 2008 - Reduce Kitt Peak 4-m data, Recalibrate Keck data, EPS of optical data constrained by AGN to host galaxy light fraction, Chandra proposal (Other), Begin Paper II (EPS of optical data), Continue with Dissertation (Chapter 3)

Fall 2008 - Travel?: Porto Alegre, Brazil (M. Brotherton, Collaboration), Riverside, CA (G. Canalizo, EPS Tutorial), Finish analysis (AGN and starburst demographics) for and writing Paper II (Submit to ApJ), Prepare results for AAS meeting, Continue with Dissertation (Complete Chapter 3)

Winter 2009 - Present results at Long Beach, CA AAS meeting, Reduce Spitzer data, IR diagnostics (Color and PAH features), Begin Paper III (IR diagnostics), Continue with Dissertation (Chapter 4)

Spring 2009 - Finish IR diagnostics analysis (Color and PAH features), Complete Paper III (Submit to ApJ), Continue with Dissertation (Complete Chapter 4), Travel? China (Z. Shang, Collaboration

Summer 2009 - Collect data of other classes of objects and modeling, Herschel proposal (Other), Begin writing Paper IV (Comparisons of PSQs with objects and models), Teach a summer Astronomy 1050 Course, Continue with Dissertation (Chapters 5 and Other)

Fall 2009 - Finish analysis for and writing Paper IV, Job search and applications, Continue with Dissertation (Complete Chapter 5), Begin final analysis

Winter 2010 - Wrap up ‘Other’ if necessary, Job search and applications, Continue with Dissertation (Complete Final Chapters), Prepare for Dissertation Defense and AAS Meeting

Spring 2010 - Defend Dissertation and present at AAS Meeting, Get a Job!

ReferencesReferences

Bahcall, J., Kirhakos, S., Schneider, D. 1996Bennert, N. et al. 2008Brotherton, M. et al. 1999Brotherton, M. et al. 2001Brotherton , M. et al. 2002Brotherton , M. et al. 2008a, in preparationBrotherton , M. et al. 2008b, in preparationBruzual & Charlot, 2001Canalizo, G. et al. 2007Di Matteo, Springel & Hernquist 2005Gebhardt, K. et al. 2000Hopkins, P. et al. 2007Toomre, A. 1977Valdes, F. et al. 2004http://antwrp.gsfc.nasa.gov/apod/ap971022.htmlhttp://astronomy.swin.edu.au/cosmos/H/Hierarchical+Merginghttp://www.utahskies.org/report/20021018/20021018weekly.html

Bahcall, J., Kirhakos, S., Schneider, D. 1996Bennert, N. et al. 2008Brotherton, M. et al. 1999Brotherton, M. et al. 2001Brotherton , M. et al. 2002Brotherton , M. et al. 2008a, in preparationBrotherton , M. et al. 2008b, in preparationBruzual & Charlot, 2001Canalizo, G. et al. 2007Di Matteo, Springel & Hernquist 2005Gebhardt, K. et al. 2000Hopkins, P. et al. 2007Toomre, A. 1977Valdes, F. et al. 2004http://antwrp.gsfc.nasa.gov/apod/ap971022.htmlhttp://astronomy.swin.edu.au/cosmos/H/Hierarchical+Merginghttp://www.utahskies.org/report/20021018/20021018weekly.html

Just in CaseJust in Case

Evolutionary SchemaEvolutionary Schema

Hopkins et al. 2007

PSQs and Prototype UN J1025-0040

PSQs and Prototype UN J1025-0040

Brotherton et al. 1999 Brotherton et al. 2002

• Quasar to host galaxy light fraction• Constrain on evolutionary stellar population synthesis models (EPS)• Quasar and host demographics: MBH, L/LEdd, SB age, SB mass

• Quasar to host galaxy light fraction• Constrain on evolutionary stellar population synthesis models (EPS)• Quasar and host demographics: MBH, L/LEdd, SB age, SB mass

Brotherton et al. 1999