The Wfc3 Infrared Spectroscopic Parallel (Wisp) Survey

Atek, Hakim; Malkan, Matthew A.; McCarthy, Patrick J.; Teplitz, Harry I.; Scarlata, Claudia; Siana, Brian; Henry, Alaina; Colbert, James; Ross, Nathaniel; Bridge, Carrie; Bunker, Andrew J.; Dressler, Alan; Fosbury, R. A. E.; Martin, Crystal L.; Shim, Hyunjin

doi:10.1088/0004-637x/723/1/104

Cited by 154 publications

(203 citation statements)

References 61 publications

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“…The misclassification of distant Seyferts will be exacerbated by the fact that at higher redshifts, most host galaxies will have much higher SFRs than they do currently, which will produce emission lines that can more easily outshine those of the active nucleus. It may be possible to overcome this problem, and identify the line emission produced by the AGN with spectroscopy at higher spatial resolution, as is possible, for example, with the Hubble Space Telescope (e.g., Atek et al 2010;Trump et al 2011). …”

Section: Discussionmentioning

confidence: 99%

Hα IMAGING OF NEARBY SEYFERT HOST GALAXIES

Theios

Malkan

Ross

2016

ApJ

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We used narrowband (Δλ=70 Å) interference filters with the CCD imaging camera on the Nickel 1.0 m telescope at Lick Observatory to observe 31 nearby (z<0.03) Seyfert galaxies in the 12 μm active galaxy sample. We obtained pure emission-line images of each galaxy, which reach down to a flux limit of 7.3×10 −15 erg cm −2 s −1 arcsec −2 , and corrected these images for [N II] emission and extinction. We separated the Hα emission line of the "nucleus" (central 100-1000 pc) from that of the host galaxy. The extended Hα emission is expected to be powered by newly formed hot stars, and indeed correlates well with other indicators of current star formation rates (SFRs) in these galaxies: extended 7.7 μm polycyclic aromatic hydrocarbon, total farinfrared, and radio luminosity. Relative to what would be expected from recent star formation, there is a 0.8 dex excess of radio emission in our Seyfert galaxies. The Hα luminosity we measured in the centers of our galaxies is dominated by the active galactic nucleus (AGN), and is linearly correlated with the hard X-ray luminosity. There is, however, an upward offset of 1 dex in this correlation for the Seyfert 1s, because their nuclear Hα emission includes a strong additional contribution from the broad-line region. We found a correlation between SFR and AGN luminosity. In spite of selection effects, we concluded that the absence of bright Seyfert nuclei in galaxies with low SFRs is real, albeit only weakly significant. Finally, we used our measured spatial distributions of Hα emission to determine what these Seyfert galaxies would look like when observed through fixed apertures (e.g., a spectroscopic fiber) at high redshifts. We found that although all of these Seyfert galaxies would be detectable emission-line galaxies at any redshift, most of them would appear to be dominated by (>67%) their HII region emission. Only the most luminous AGNs (log(L Hα /erg s −1 )>41.5) would still be identified as such at z∼0.3.

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Section: Discussionmentioning

confidence: 99%

Hα IMAGING OF NEARBY SEYFERT HOST GALAXIES

Theios

Malkan

Ross

2016

ApJ

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“…We note that the following two samples are biased because they were both selected to address specific star-forming populations. Atek et al (2014) presented the properties (stellar masses and SFRs) of 1034 galaxies at 0.3 < z < 2.3 selected through emission lines with the WISP (Atek et al 2010) and 3DHST surveys. This selection favours the detection of starburst galaxies.…”

Section: Other Star-forming Galaxy Samplesmentioning

confidence: 99%

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

Japelj

Vergani

Salvaterra

et al. 2016

A&A

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100

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Aims. Long gamma-ray bursts (LGRBs) are associated with the deaths of massive stars and might therefore be a potentially powerful tool for tracing cosmic star formation. However, especially at low redshifts (z < 1.5) LGRBs seem to prefer particular types of environment. Our aim is to study the host galaxies of a complete sample of bright LGRBs to investigate the effect of the environment on GRB formation. Methods. We studied host galaxy spectra of the Swift/BAT6 complete sample of 14 z < 1 bright LGRBs. We used the detected nebular emission lines to measure the dust extinction, star formation rate (SFR), and nebular metallicity (Z) of the hosts and supplemented the data set with previously measured stellar masses M . The distributions of the obtained properties and their interrelations (e.g. mass-metallicity and SFR-M relations) are compared to samples of field star-forming galaxies. Results. We find that LGRB hosts at z < 1 have on average lower SFRs than if they were direct star formation tracers. By directly comparing metallicity distributions of LGRB hosts and star-forming galaxies, we find a good match between the two populations up to 12 + log O H ∼ 8.4−8.5, after which the paucity of metal-rich LGRB hosts becomes apparent. The LGRB host galaxies of our complete sample are consistent with the mass-metallicity relation at similar mean redshift and stellar masses. The cutoff against high metallicities (and high masses) can explain the low SFR values of LGRB hosts. We find a hint of an increased incidence of starburst galaxies in the Swift/BAT6 z < 1 sample with respect to that of a field star-forming population. Given that the SFRs are low on average, the latter is ascribed to low stellar masses. Nevertheless, the limits on the completeness and metallicity availability of current surveys, coupled with the limited number of LGRB host galaxies, prevents us from investigating more quantitatively whether the starburst incidence is such as expected after taking into account the high-metallicity aversion of LGRB host galaxies.

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“…Rest-frame UV spectra have been measured for ∼ 3000 galaxies at 1.5 ≤ z ≤ 3.5 (Steidel et al , 2004), yet the sample of such objects is biased towards relatively blue, star-forming galaxies, and these spectra are primarily sensitive to interstellar and circumgalactic medium (ISM/CGM) features tracing outflowing gas (e.g., Shapley et al 2003). Current surveys with the HST/WFC3 near-IR grisms are yielding rest-frame optical spectra of ∼ 10, 000 galaxies at z > 1 (Brammer et al 2012;Atek et al 2010), yet the low resolution (R < 130) and limited wavelength range (λ < 1.6µm) prevent a robust characterization of emission and absorption line ratios and widths over the range 1.5 z 3.5. Finally, moderate-resolution rest-frame optical spectroscopy has been obtained at 1.5 z 3.5 for (UV-selected) starforming galaxies (e.g., Erb et al 2006;Mannucci et al 2009;Förster Schreiber et al 2009) and stellar masslimited samples of massive galaxies (M ≥ 10 11 M ⊙ ; e.g., Kriek et al 2008b).…”

Section: Introductionmentioning

confidence: 99%

THE MOSFIRE DEEP EVOLUTION FIELD (MOSDEF) SURVEY: REST-FRAME OPTICAL SPECTROSCOPY FOR ∼1500 H -SELECTED GALAXIES AT $1.37\leqslant z\leqslant 3.8$

Kriek

Shapley

Reddy

et al. 2015

ApJS

439

521

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In this paper we present the MOSFIRE Deep Evolution Field (MOSDEF) survey. The MOSDEF survey aims to obtain moderate-resolution (R = 3000 − 3650) rest-frame optical spectra (∼ 3700 − 7000Å) for ∼1500 galaxies at 1.37 ≤ z ≤ 3.80 in three well-studied CANDELS fields: AEGIS, COSMOS, and GOODS-N. Targets are selected in three redshift intervals: 1.37 ≤ z ≤ 1.70, 2.09 ≤ z ≤ 2.61, and 2.95 ≤ z ≤ 3.80, down to fixed H AB (F160W) magnitudes of 24.0, 24.5 and 25.0, respectively, using the photometric and spectroscopic catalogs from the 3D-HST survey. We target both strong nebular emission lines (e.g.,, 6585, and [S ii] λλ6718, 6733) and stellar continuum and absorption features (e.g., Balmer lines, Ca-ii H and K, Mgb, 4000Å break). Here we present an overview of our survey, the observational strategy, the data reduction and analysis, and the sample characteristics based on spectra obtained during the first 24 nights. To date, we have completed 21 masks, obtaining spectra for 591 galaxies. For ∼80% of the targets we derive a robust redshift from either emission or absorption lines. In addition, we confirm 55 additional galaxies, which were serendipitously detected. The MOSDEF galaxy sample includes unobscured star-forming, dusty star-forming, and quiescent galaxies and spans a wide range in stellar mass (∼ 10 9 − 10 11.5 M ⊙ ) and star formation rate (∼ 10 0 − 10 3 M ⊙ yr −1 ). The spectroscopically confirmed sample is roughly representative of an H-band limited galaxy sample at these redshifts. With its large sample size, broad diversity in galaxy properties, and wealth of available ancillary data, MOSDEF will transform our understanding of the stellar, gaseous, metal, dust, and black hole content of galaxies during the time when the universe was most active.

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The Wfc3 Infrared Spectroscopic Parallel (Wisp) Survey

Cited by 154 publications

References 61 publications

Hα IMAGING OF NEARBY SEYFERT HOST GALAXIES

Hα IMAGING OF NEARBY SEYFERT HOST GALAXIES

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of theSwift/BAT6 complete sample of bright LGRBs

THE MOSFIRE DEEP EVOLUTION FIELD (MOSDEF) SURVEY: REST-FRAME OPTICAL SPECTROSCOPY FOR ∼1500 H -SELECTED GALAXIES AT $1.37\leqslant z\leqslant 3.8$

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