THE WFC3 INFRARED SPECTROSCOPIC PARALLEL (WISP) SURVEY

被引：122

作者：

Atek, H. ^{[1
]}

Malkan, M. ^{[2
]}

McCarthy, P. ^{[3
]}

Teplitz, H. I. ^{[4
]}

Scarlata, C. ^{[1
]}

Siana, B. ^{[5
]}

Henry, A. ^{[6
]}

Colbert, J. W. ^{[1
]}

Ross, N. R. ^{[2
]}

Bridge, C. ^{[5
]}

Bunker, A. J. ^{[7
]}

Dressler, A. ^{[3
]}

Fosbury, R. A. E. ^{[8
]}

Martin, C. ^{[6
]}

Shim, H. ^{[1
]}

机构：

[1] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA

[2] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90024 USA

[3] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA

[4] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA

[5] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[6] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[7] Univ Oxford, Dept Phys, Oxford OX1 3RH, England

[8] European So Observ, Space Telescope European Coordinating Facil, D-8046 Garching, Germany

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 723卷 / 01期

关键词：

galaxies: distances and redshifts; galaxies: statistics; infrared: galaxies; surveys; EMISSION-LINE GALAXIES; ULTRA-DEEP-FIELD; STAR-FORMING GALAXIES; MASS-METALLICITY RELATION; LY-ALPHA EMITTERS; FRAME OPTICAL-SPECTRA; EXTREMELY RED OBJECTS; REDSHIFT SURVEY; LUMINOSITY FUNCTION; ACS GRISM;

D O I：

10.1088/0004-637X/723/1/104

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the WFC3 Infrared Spectroscopic Parallel (WISP) Survey. WISP is obtaining slitless, near-infrared grism spectroscopy of similar to 90 independent, high-latitude fields by observing in the pure-parallel mode with the Wide Field Camera Three on the Hubble Space Telescope for a total of similar to 250 orbits. Spectra are obtained with the G(102) (lambda = 0.8-1.17 mu m, R similar to 210) and G(141) grisms (lambda = 1.11-1.67 mu m, R similar to 130), together with direct imaging in the J and H bands (F110W and F140W, respectively). In the present paper, we present the first results from 19 WISP fields, covering approximately 63 arcmin(2). For typical exposure times (similar to 6400 s in G(102) and similar to 2700 s in G(141)), we reach 5 sigma detection limits for emission lines of f similar to 5 x 10(-17) erg s(-1) cm(-2) for compact objects. Typical direct imaging 5 sigma limits are 26.3 and 26.1 mag. (AB) in F110W and F140W, respectively. Restricting ourselves to the lines measured with the highest confidence, we present a list of 328 emission lines, in 229 objects, in a redshift range 0.3 < z < 3. The single-line emitters are likely to be a mix of H alpha and [O III]5007,4959 angstrom, with H alpha predominating. The overall surface density of high-confidence emission-line objects in our sample is approximately 4 per arcmin2. These first fields show high equivalent width sources, active galactic nucleus, and post-starburst galaxies. The median observed star formation rate (SFR) of our H alpha-selected sample is 4 M-circle dot yr(-1). At intermediate redshifts, we detect emission lines in galaxies as faint as H-140 similar to 25, or M-R < -19, and are sensitive to SFRs down to less than 1 M-circle dot yr(-1). The slitless grisms on WFC3 provide a unique opportunity to study the spectral properties of galaxies much fainter than L* at the peak of the galaxy assembly epoch.

引用

页码：104 / 115

页数：12

共 68 条

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