Merging Galaxies in GOODS-S: First Extragalactic Results from Keck Laser Adaptive Optics

Melbourne, J.; Wright, Shelley A.; Barczys, M.; Bouchez, Antonin H.; Chin, Jason C. Y.; Dam, Marcos A. van; Hartman, Scott; Johansson, Erik M. J.; Koo, David C.; Lafon, Robert E.; Larkin, James E.; Mignant, D. Le; Lotz, Jennifer M.; Max, C. E.; Pennington, D. M.; Stomski, Paul J.; Summers, Douglas M.; Wizinowich, Peter

doi:10.1086/430830

Cited by 40 publications

(51 citation statements)

References 26 publications

(20 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The unique new data that the WFC3 IR channel can provide are high-resolution, very sensitive near-IR photometry over fields larger than those possible with HST NICMOS, or over wide fields with adaptive optics from the ground (e.g., Steinbring et al 2004;Melbourne et al 2005).…”

Section: The Ers Filter Setmentioning

confidence: 99%

THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2-2 μm WAVELENGTH

Windhorst

Cohen

Hathi

et al. 2011

ApJS

271

298

View full text Add to dashboard Cite

We describe the Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) Early Release Science (ERS) observations in the Great Observatories Origins Deep Survey (GOODS) South field. The new WFC3 ERS data provide calibrated, drizzled mosaics in the UV filters F225W, F275W, and F336W, as well as in the near-IR filters F098M (Y s ), F125W (J), and F160W (H) with 1-2 HST orbits per filter. Together with the existing HST Advanced Camera for Surveys (ACS) GOODS-South mosaics in the BViz filters, these panchromatic 10-band ERS data cover 40-50 arcmin 2 at 0.2-1.7 μm in wavelength at 0. 07-0. 15 FWHM resolution and 0. 090 Multidrizzled pixels to depths of AB 26.0-27.0 mag (5σ ) for point sources, and AB 25.5-26.5 mag for compact galaxies. In this paper, we describe (1) the scientific rationale, and the data taking plus reduction procedures of the panchromatic 10-band ERS mosaics, (2) the procedure of generating object catalogs across the 10 different ERS filters, and the specific star-galaxy separation techniques used, and (3) the reliability and completeness of the object catalogs from the WFC3 ERS mosaics. The excellent 0. 07-0. 15 FWHM resolution of HST/WFC3 and ACS makes star-galaxy separation straightforward over a factor of 10 in wavelength to AB 25-26 mag from the UV to the near-IR, respectively. Our main results are: (1) proper motion of faint ERS stars is detected over 6 years at 3.06 ± 0.66 mas year −1 (4.6σ ), consistent with Galactic structure models; (2) both the Galactic star counts and the galaxy counts show mild but significant trends of decreasing count slopes from the mid-UV to the near-IR over a factor of 10 in wavelength; (3) combining the 10-band ERS counts with the panchromatic Galaxy and Mass Assembly survey counts at the bright end (10 mag AB 20 mag) and the Hubble Ultra Deep Field counts in the BV izY s J H filters at the faint end (24 mag AB 30 mag) yields galaxy counts that are well measured over the entire flux range 10 mag AB 30 mag for 0.2-2 μm in wavelength; (4) simple luminosity+density evolution models can fit the galaxy counts over this entire flux range. However, no single model can explain the counts over this entire flux range in all 10 filters simultaneously. More sophisticated models of galaxy assembly are needed to reproduce the overall constraints provided by the current panchromatic galaxy counts for 10 mag AB 30 mag over a factor of 10 in wavelength.

show abstract

Section: The Ers Filter Setmentioning

confidence: 99%

THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2-2 μm WAVELENGTH

Windhorst

Cohen

Hathi

et al. 2011

ApJS

271

298

View full text Add to dashboard Cite

show abstract

“…Melbourne et al 2005, Davidge et al 2005. The corresponding linear scale is ∼ 5 pc(D/10Mpc); at the distance of the Virgo cluster (D ≈ 16 Mpc), resolving r h is only possible in galaxies with M • > ∼ 10 8 M ⊙ (Eq.…”

Section: Structural Properties Of Galaxies and Nucleimentioning

confidence: 99%

Dynamics of galaxy cores and supermassive black holes

2006

View full text Add to dashboard Cite

show abstract

“…A field near guide star GOODS-S19 was observed for 3 hr in 2004 October. The resulting images of merging galaxies have been published in Melbourne et al (2005). Solar system engineering science projects have included measuring the system mass of binary Trojan asteroids (Marchis et al 2005) and Kuiper Belt objects (Brown et al 2005).…”

Section: Science Demonstration Programmentioning

confidence: 99%

The W. M. Keck Observatory Laser Guide Star Adaptive Optics System: Overview

Wizinowich

Mignant

Bouchez

et al. 2006

PUBL ASTRON SOC PAC

426

198

View full text Add to dashboard Cite

ABSTRACT. The Keck Observatory began science observations with a laser guide star adaptive optics system, the first such system on an 8-10 m class telescope, in late 2004. This new capability greatly extends the scientific potential of the Keck II Telescope, allowing near-diffraction-limited observations in the near-infrared using natural guide stars as faint as 19th magnitude. This paper describes the conceptual approach and technical implementation followed for this system, including lessons learned, and provides an overview of the early science capabilities.

show abstract

Merging Galaxies in GOODS-S: First Extragalactic Results from Keck Laser Adaptive Optics

Cited by 40 publications

References 26 publications

THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2-2 μm WAVELENGTH

THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2-2 μm WAVELENGTH

Dynamics of galaxy cores and supermassive black holes

The W. M. Keck Observatory Laser Guide Star Adaptive Optics System: Overview

Contact Info

Product

Resources

About