GRAPES, Grism Spectroscopy of the Hubble Ultra Deep Field: Description and Data Reduction

Pirzkal, Norbert; Xu, Chun; Malhotra, Sangeeta; Rhoads, James E.; Koekemoer, Anton M.; Moustakas, Leonidas A.; Walsh, J. R.; Windhorst, Rogier A.; Daddi, E.; Cimatti, A.; Ferguson, Henry C.; Gardner, Jonathan P.; Grönwall, C.; Haiman, Zoltán; Kümmel, M.; Panagia, N.; Pasquali, A.; Stiavelli, M.; Alighieri, S. di Serego; Tsvetanov, Z.; Vernet, J.; Yan, Hao

doi:10.1086/422582

Cited by 117 publications

(109 citation statements)

References 15 publications

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“…Spectra of galaxies in the GOODS-South field were obtained by several different observational campaigns: the two most extended ones were conducted by ESO with FORS2 (Vanzella et al 2006(Vanzella et al , 2008(Vanzella et al , 2009) and VIMOS (Popesso et al 2009). Other redshifts were obtained with the VLT by GMASS (Kurk et al 2009), by the HST/ACS/G880L grism survey PEARS (Straughn et al 2008) and the similar GRAPES project (Pirzkal et al 2004;Malhotra et al 2005). In total there are 130 U-dropout galaxies with confirmed redshift.…”

Section: The Samplementioning

confidence: 99%

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Pentericci¹,

Grazian²,

Scarlata

et al. 2010

A&A

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Aims. We investigate the physical and morphological properties of Lyman break galaxies (LBGs) at redshift ∼2.5 to ∼3.5, to determine if and how they depend on the nature and strength of the Lyα emission. Methods. We selected U-dropout galaxies from the z-detected GOODS-MUSIC catalog by adapting the classical Lyman break criteria on the GOODS filter set. We kept only those galaxies with spectroscopic confirmation, mainly from VIMOS and FORS public observations. Using the full multi-wavelength 14-bands information (U to IRAC), we determined the physical properties of the galaxies through a standard spectral energy distribution fitting procedure with the updated Charlot & Bruzual (2009) templates. We also added other relevant observations of the GOODS field, i.e. the 24 μm observations from Spitzer/MIPS and the 2 MSec Chandra X-ray observations. Finally, using non parametric diagnostics (Gini, Concentration, Asymmetry, M 20 and ellipticity), we characterized the rest-frame UV morphologies of the galaxies. We then analyzed how these physical and morphological properties correlate with the presence of the Lyα emission line in the optical spectra. Results. We find that unlike at higher redshift, the dependence of physical properties on the Lyα line is milder: galaxies without Lyα in emission tend to be more massive and dustier than the rest of the sample, but all other parameters, ages, star formation rates (SFR), X-ray emission and UV morphology do not depend strongly on the presence of the Lyα emission. A simple scenario where all LBGs have intrinsically high Lyα emission, but where the dust and neutral hydrogen content (which shapes the final appearance of the Lyα) depend on the mass of the galaxies, is able to reproduce the majority of the observed properties at z ∼ 3. Some modification might be needed to account for the observed evolution of these properties with cosmic epoch, which is also discussed.

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Section: The Samplementioning

confidence: 99%

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Pentericci¹,

Grazian²,

Scarlata

et al. 2010

A&A

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“…Seven of these galaxies belong to a large scale structure at z = 1.61 that is discussed in a companion paper (Kurk et al 2007b). Ten spectra were obtained with an integration time of 30 h each, whereas three (IDs 2111, 2239, 2559) were repeated in two independent masks and each of them accumulated an integration time of 60 h. The two galaxies located within the HUDF (IDs 472 and 996) were also consistently identified by Daddi et al (2005a) (their IDs 3650 and 8238 respectively) using HST+ACS slitless grism spectroscopy (GRAPES project; Pirzkal et al 2004 Kennicutt (1998), we derive SFR ≈ 1-4 M yr −1 for the four galaxies with [OII]λ3727 emission (see Table 1). If dust extinction is present, these SFRs are lower limits.…”

Section: Spectroscopic Selection and Propertiesmentioning

confidence: 99%

GMASS ultradeep spectroscopy of galaxies atz~ 2

Cimatti¹,

Cassata

Pozzetti

et al. 2008

A&A

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513

662

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Aims. The aim of this work is to investigate the physical, structural and evolutionary properties of old, passive galaxies at z > 1.4 and to place new constraints on massive galaxy formation and evolution. Methods. We combine ultradeep optical spectroscopy from the GMASS project (Galaxy Mass Assembly ultradeep Spectroscopic Survey) with GOODS multi-band (optical to mid-infrared) photometry and HST imaging to study a sample of spectroscopically identified passive galaxies at 1.39 < z < 1.99 selected from Spitzer Space Selescope imaging at 4.5 µm. Results. A stacked spectrum with an equivalent integration time of ∼500 h was obtained and compared with libraries of synthetic stellar population spectra. The stacked spectrum is publicly released. The spectral and photometric SED properties indicate very weak or absent star formation, moderately old stellar ages of ≈1 Gyr (for solar metallicity) and stellar masses in the range of 10 10−11 M , thus implying that the major star formation and assembly processes for these galaxies occurred at z > 2. No X-ray emission was found neither from individual galaxies nor from a stacking analysis of the sample. Only one galaxy shows a marginal detection at 24 µm. These galaxies have morphologies that are predominantly compact and spheroidal. However, their sizes (R e 1 kpc) are much smaller than those of spheroids in the present-day Universe. Their stellar mass surface densities are consequently higher by ≈1 dex if compared to spheroids at z ≈ 0 with the same mass. Their rest-frame B-band surface brightness scales with the effective radius, but the offset with respect to the surface brightness of the local Kormendy relation is too large to be explained by simple passive evolution. At z ≈ 1, a larger fraction of passive galaxies follows the z ≈ 0 size-mass relation. Superdense relics with R e ≈ 1 kpc are extremely rare at z ≈ 0 with respect to z > 1, and absent if R e < 1 kpc. Because of the similar sizes and mass densities, we suggest that the superdense passive galaxies at 1 < z < 2 are the remnants of the powerful starbursts occurring in submillimeter-selected galaxies at z > 2. The results are compared with theoretical models and the main implications discussed in the framework of massive galaxy formation and evolution.

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“…The FIGS G102 data were reduced in a manner that loosely follows the method used for the GRAPES and PEARS data (Pirzkal et al 2004). However, the planning and execution of the observations were first based on accurate simulations, which then served as the the basis for the actual extraction of the data.…”

Section: Overviewmentioning

confidence: 99%

“…The information content of a spectrum can be better described by the net significance ( ), which was introduced in Pirzkal et al (2004).  is the maximum cumulative S/N of a spectrum.…”

Section: Net Significancementioning

confidence: 99%

FIGS—Faint Infrared Grism Survey: Description and Data Reduction

Pirzkal

Malhotra

Ryan

et al. 2017

ApJ

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The Faint Infrared Grism Survey (FIGS) is a deep Hubble Space Telescope (HST) WFC3/IR (Wide Field Camera 3 Infrared) slitless spectroscopic survey of four deep fields. Two fields are located in the Great Observatories Origins Deep Survey-North (GOODS-N) area and two fields are located in the Great Observatories Origins Deep Survey-South (GOODS-S) area. One of the southern fields selected is the Hubble Ultra Deep Field. Each of these four fields were observed using the WFC3/G102 grism (0.8 μm-1.15 μm continuous coverage) with a total exposure time of 40 orbits (≈100 kilo-seconds) per field. This reaches a s 3 continuum depth of »26 AB magnitudes and probes emission lines to~---10 erg s cm 17 12 . This paper details the four FIGS fields and the overall observational strategy of the project. A detailed description of the Simulation Based Extraction (SBE) method used to extract and combine over 10,000 spectra of over 2000 distinct sources brighter than = m 26.5mag is provided. High fidelity simulations of the observations is shown to significantly improve the background subtraction process, the spectral contamination estimates, and the final flux calibration. This allows for the combination of multiple spectra to produce a final high quality, deep, 1D spectra for each object in the survey.

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GRAPES, Grism Spectroscopy of the Hubble Ultra Deep Field: Description and Data Reduction

Cited by 117 publications

References 15 publications

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

GMASS ultradeep spectroscopy of galaxies atz~ 2

FIGS—Faint Infrared Grism Survey: Description and Data Reduction

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