1 / 17

SED measurements of radio galaxies 1 < z < 5

SED measurements of radio galaxies 1 < z < 5. Bob Fosbury (ST-ECF) on behalf of the SHzRGS team Daniel Stern - PI, Peter Eisenhardt (JPL) Carlos De Breuck - Co-PI, Joel Vernet, Alessandro Rettura (ESO) Bob Fosbury (ST-ECF) Andrew Zirm (STSCI) Brigitte Rocca-Volmerange (IAP)

varick
Download Presentation

SED measurements of radio galaxies 1 < z < 5

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. SED measurements of radio galaxies 1 < z < 5 • Bob Fosbury (ST-ECF) on behalf of the SHzRGS team • Daniel Stern - PI, Peter Eisenhardt (JPL) • Carlos De Breuck - Co-PI, Joel Vernet, Alessandro Rettura (ESO) • Bob Fosbury (ST-ECF) • Andrew Zirm (STSCI) • Brigitte Rocca-Volmerange (IAP) • Nick Seymour, Mark Lacy, Harry Teplitz (SSC) • Arjun Dey, Mark Dickinson (NOAO) • Wil van Breugel, Adam Stanford (UCLLNL) • George Miley, Huub Rottgering (Leiden) • Partick McCarthy (OCIW) • Dave Alexander (IoA)

  2. Objective • The hosts of powerful radio galaxies represent the most massive galaxies at their epoch • By observing the SED through the restframe H-band with Spitzer, we measure the stellar masses • The Spitzer images allow us to investigate the (proto)-cluster environment • The SMBH is characterised from X-ray and radio measurements

  3. Evidence • gE and cD galaxies in the local universe • r^(1/4) light profiles in distant sources (NICMOS) • HzRG reside in (proto-)cluster environments • Large, luminous Ly-a halos • sub-mm detections => high star formation rates • NIR Hubble diagram (K-z; Rocca-Volmerange et al. 2004) • Correlation of stellar bulge and BH masses

  4. Sample • The objective is to cover the radio luminosity - redshift plane as uniformly as possible in the range 1 < z < 4, covering two orders of magnitude in radio luminosity • Sample chosen to maximise number of supporting observation (but no bias towards cold dust properties - 850micron Obs not Det) Solid symbols - HzRGs in our Spitzer sample with IRAC/IRS imaging Large circles - MIPS observations as well Filled circles - HzRGs with HST data Filled squares - HzRGs with SCUBA data Plusses - parent sample of 225 HzRGs from which our sample of 70 was drawn

  5. Spitzer observations • 3-camera programme: GO 3329 (Stern) • IRAC: 4x30s in all 4 bands => 5-sigma at m_AB=22 for ch 1 & 2 and at m_AB=20 for ch 3 & 4 • IRS: 16 micron imaging (peak-up) mode; 2x60s => 5_sigma at 0.17mJy • MIPS: subset of 21 sources with low 24 micron background; all three bands [24 (30s), 70 (30s), 160 (50s)] but most detections at 24

  6. Supporting observations • 48/70 have HST imaging; total exposure of 1.5Ms • 16 have Chandra/XMM-Newton data • 43 have published sub-mm data • 22 have deep optical polarimetric observations from Keck/VLT • Use to construct broadband SED and characterise AGN and dust re-radiation in addition to the evolved stellar population • Also use to study galaxy morphology and environment

  7. WFPC2 - IRAC • HST/WFPC2 [top] and Spitzer/IRAC [bottom] images of 5 HzRGs • From left to right, galaxies shown are 3C266 (z = 1.275), MRC 0152-209 (z = 1.920), USS 1707+105 (z = 2.349), MRC 0406-244 (z = 2.427), and 4C+41.17 (z = 3792) • Images are 30 arcsec on a side, oriented with North up and East to the left. Note that a number of the fields show overdensities of infrared-bright, optically-faint galaxies

  8. Supporting proposals • ESO and Palomar imaging (for 4000Å-break) • IRS mid-IR spectroscopy (Silicate, PAH and continuum) • MIPS - to extend subset • ESO imaging polarimetry (removal of AGN component) • MAMBO and SCUBA sub-mm • VLA 4.8 and 8.4 GHz to extend 3 GHz restframe depth: polarimetry to measure RM environment • HST archive

  9. 4C+23.56 • This is our initial example object with very complete observational coverage.

  10. Keck spectropolarimetry • Showing the dominance of the scattered quasar in the restframe ultraviolet(Cimatti et al. 1998;Vernet et al. 2001)

  11. Composite SED

  12. SED modelling • Initial modelling with stellar population (PEGASE.2), hot and cold dust (Siebenmorgen), and synchrotron components • Will add the scattered AGN • We need deeper sum-mm observations for most of this sample

  13. Restframe H-band estimates • By Nick Seymour (elliptical templates +warm dust) • Full SED fitting tbd by Alessandro Rettura

  14. Restframe H-band vs. z • Derived from best-fit models to the multi-band photometry • Sources with large error bars lack MIPS 24micron observations, making the decomposition of stellar and dust/AGN components of the SED less secure. • The error bars for these sources show that the range of reasonable stellar luminosities given (1) the total H-band luminosity and (2) that the stellar emission typically dominates at observed 3.6micron (as seen in the modelling of sources with MIPS data) and hence can predict a reasonable lower value to the H-band luminosity. • The red line shows the expected H-band luminosity of a passively evolving 10^12M_sun elliptical galaxy from the PEGASE.2 models (see Rocca-Volmerange et al., 2004)

  15. First cut at M-z for Radio Galaxy hosts

  16. BH mass vs. stellar mass • Local galaxies with measured kinematic and stellar masses (blue stars) • HzRG with measured X-ray luminosities (red squares) • Implications for BH growth at early epochs

  17. Nick Seymour’s status pages

More Related