1 / 21

May 21, 2005 David Schiminovich Michel Zamojski Columbia University M. Rich UCLA +

GALEX and COSMOS: Morphologies of Star-Forming Galaxies out to z~1. GALEX Galaxy Evolution Explorer An Ultraviolet Imaging and Spectroscopic Survey. May 21, 2005 David Schiminovich Michel Zamojski Columbia University M. Rich UCLA + GALEX and COSMOS teams. FUV. FUV. NUV. NUV. I814W.

kuniko
Download Presentation

May 21, 2005 David Schiminovich Michel Zamojski Columbia University M. Rich UCLA +

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. GALEX and COSMOS: Morphologies of Star-Forming Galaxies out to z~1 GALEX Galaxy Evolution Explorer An Ultraviolet Imaging and Spectroscopic Survey May 21, 2005 David Schiminovich Michel Zamojski Columbia University M. Rich UCLA + GALEX and COSMOS teams

  2. FUV FUV NUV NUV I814W I814W z=0.7 GALEX vs. COSMOS GALEX Bands FUV (1530 A) NUV (2310 A) GALEX FOV: 1.2 deg. diam PSF: 5” (FWHM) SSP - Bruzual and Charlot (2003) COSMOS KYOTO

  3. GALEX/COSMOS Field Deep Imaging Survey Obs. Spring 2004 4 targets in region on 0.5 degree grid 50 ks each 100, 150, 200 ks in overlap regions mAB <25-26 01 03 02 04 1.4O COSMOS KYOTO

  4. Observing Status - Spring 05 (IR1.1) • Central pointing (COSMOS_00) • Shallow imaging (~3 ks processed) • Shallow grism spectroscopy (~20 ks) • candidate for deeper follow-up • No additional COSMOS observations in Spring 05 • Schedule availability limited • Spectroscopy observations given lower priority • GALEX FUV detector off COSMOS KYOTO

  5. Processing Status - April 05 (IR1.1) • Integration time on four fields (target was 50ks): • COSMOS_01 - 44024 s • COSMOS_02 - 44442 s • COSMOS_03 - 41270 s • COSMOS_04 - 44169 s • (85-90% observed data passed checks) • Catalog Refinements • Source confusion/deblending • Background Subtraction - faint source photometry • Significant progress has been made in these areas COSMOS KYOTO

  6. 10’ COSMOS KYOTO

  7. GALEX/COSMOS Field Green Contours: GALEX NUV Image: COSMOS ACS COSMOS KYOTO

  8. GALEX Data Release Plan GALEX/COSMOS images and catalogs will be released to public as part of GALEX GR2 (second data release) in late Fall 2005 Pipeline outputs only Will also be provided to IRSA at that time GALEX has suffered serious funding cut, and FUV problems which affects our ability to process the COSMOS images. COSMOS KYOTO

  9. GALEX/COSMOS Catalog • New GALEX/COSMOS matched catalog using latest COSMOS photo-z cat (05/2005) • Photometry using optical prior (positions only) • Michel Zamojski (grad student at Columbia) performing reduction/analysis • Can provide catalogs and images for COSMOS projects (or participation in analysis effort) upon request. COSMOS KYOTO

  10. GALEX/COSMOS Science GALEX+VVDS Schiminovich et al (2005) GALEX+SDSS - Seibert et al 2005 COSMOS KYOTO

  11. GALEX/COSMOS Science Nearly 100,000 galaxies have been detected by GALEX down to NUV~25.5 over the full field. COSMOS has no better tracer of SFR in the range 0<z<1 than the GALEX FUV and NUV observations (even w/ caveats of dust attenuation and SFH) COSMOS KYOTO

  12. Short-term GALEX/COSMOS Projects • Morphological Properties of Star-Forming Galaxies at 0.5<z<1.0 using COSMOS/GALEX(Zamojski, DS, Rich et al) • Apj Letter part of Zamojski PhD thesis (also see next few slides) • Overall project combines other local and deep data sets. For this reason Michel has measured his own morphologies • Willing to distribute morph. catalog to team and/or use other morph. catalogs for some analysis • Comparison morphologies in ugriz have been measured using SDSS NYU low-z galaxy catalog (can also provide to team) • GALEX Far and Near Ultraviolet Observations of the HST/COSMOS Survey Region (DS, Zamojski, Rich et al) • Basic description of GALEX observations, properties and initial analysis) • Letter + Paper will be distributed to team/ready for submission in August COSMOS KYOTO

  13. GALEX/COSMOS Projects (~1 yr) • Morphological evolution of star-forming galaxies and the evolution of rest-frame ultraviolet luminosity function/density vs. morphological type. (Zamojski, DS, Rich, et al) • Physical properties of star-forming galaxies at 0.5<z<1.0 (Rich, Salim, DS, et al) • SFR/Mass vs. morphology (DS, Rich et al) • Morphological properties of galaxies at SF extremes (starburst/LBGs, ~k+a/red objects) (Rich, DS et al) • Evolution of UV extinction properties and dependence on morphological type, size. (would be excellent to combine w/ VLA/COSMOS, possibly X-ray and some Spitzer data) • Evolution of UV luminosity/SFR vs. density/local environment COSMOS KYOTO

  14. GALEX/COSMOS Analysis Over full 2 sq. deg: >75k GALEX matches w/ optical data NUV<25 Analysis for 1 sq. deg: (using Dec/Jan photo-z and Cycle 12 ACS data) High S/N I-limited sample with I<23 and good photo-zs (17k objects) NUV<25 (9k galaxies) Redshift Range: 0.55<z<0.8 Quantities measured: GALEX: MFUV, LFUV ACS: Morphology, r50 COSMOS KYOTO

  15. Morphology of FUV luminous vs. FUV faint galaxies at 0.55<z<0.8 • Non-parametric morphologies: • Concentration (C) B/D, Type • Asymmetry (A) Merger • Clumpiness (S) Star Formation • Gini Coefficient (G) B/D, Type • M20 (M20) B/D, Merger • following work of Abraham et al (1996), Conselice (2003), Lotz et al (2004) • 17000 total CASGM measurements from ACS/COSMOS data • 5540 in redshift slice 0.55<z<0.8 COSMOS KYOTO

  16. I. Morphology of FUV luminousvs. FUV underluminous galaxies at 0.55<z<0.8 MFUV < -18 MFUV > -18 2.5k galaxies each bin

  17. COSMOS rest frame V-band half-light radius (squares) II. Sizes of extreme UV-luminous galaxies Local Measurement: Heckman, Hoopes et al (2005) LFUV,bol > 2x1010 Msol SFR 5-50 Msol/yr SDSS u-band half-light radius (circles) Compact galaxies may be LBG analogs with high SFR/area and SFR/<SFR> Large galaxies may be extreme disks Large Compact COSMOS KYOTO

  18. Compact UV Luminous Galaxies (UVLGs) r50~2.5 kpc 0.55<z<0.8 COSMOS KYOTO

  19. Large UV Luminous Galaxies (UVLGs) r50~10 kpc 0.55<z<0.8 COSMOS KYOTO

  20. Conclusions and Work in Progress • GALEX has performed deep imaging entire 2 sq. deg. COSMOS field • At 0.55<z<0.8, FUV luminous galaxies have higher Concentration, Clumpiness, Gini Coefficient, M20 (and somewhat higher Asymmetry) than their FUV faint counterparts. • At 0.55<z<0.8, UVLGs (extreme UV luminous galaxies) have half-light radii roughly consistent with range seen in local sample, where both compact and large galaxies are seen. Locus slightly higher than for typical LBG. Work in Progress • Further investigation into relation between morphology, SFR and mass and evolution w/ z. • Morphologies of local comparison sample

  21. Of General Interest … • GALEX photometry could be used to constrain better the photo z’s especially for star forming galaxies z<1.5 • Would be useful to have final throughput bandpasses as a function of  for all optical/IR flux points >> Salim’s physical parameters (masses, SFR, etc.). Can this be made available on web site? • We could add these derived parameters to the data set. • Should a U-cosmos proposal to “finish” Galex photometry of the field and to add ~200 ksec of spectroscopy be proposed?

More Related