Star Formation Rate Indicators in the Sloan Digital Sky Survey

Hopkins, A. M.; Miller, C. J.; Nichol, R. C.; Connolly, Andrew J.; Bernardi, Mariangela; Gómez, Percy; Goto, Tomotsugu; Tremonti, Christy; Brinkmann, J.; Ivezić, Željko; Lamb, D. Q.

doi:10.1086/379608

Cited by 356 publications

(560 citation statements)

References 65 publications

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“…This results in the lower SFRs in PKS1138 (third point). The fourth point can then be easily understood given the correlation between between SFR and dust amount (lower SFR galaxies have less dust, e.g., Hopkins et al 2003).…”

Section: Discussionmentioning

confidence: 99%

The environmental dependence of galaxy properties atz = 2

Tanaka¹,

Breuck²,

Venemans³

et al. 2010

A&A

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We report on the environmental dependence of galaxy properties at z = 2.15. We construct multi-band photometric data sets in the (proto-)cluster PKS1138-26 field and in the GOODS field. We then fit spectral energy distributions of the galaxies with model templates generated with the latest stellar population synthesis code and derive physical properties of galaxies from the fits. To quantify the environmental dependence of galaxy properties, a special care is taken of systematic errors -we use data sets that have almost the same wavelength samplings, use the same code to fit SEDs with the same set of templates, and compare relative differences between the two samples. We find that the PKS1138 galaxies have similar ages, shorter star formation time scales, lower star formation rates, and weaker dust extinction compared to the GOODS galaxies at z ∼ 2. This trend is similar to that observed locally, suggesting that the environmental dependence of galaxy properties is already partly in place as early as z = 2.15. We show that the PKS1138 galaxies assemble the bulk of their masses ∼1 Gyr earlier than field galaxies, i.e., the galaxy formation depends on environment. Galaxy mergers should frequently occur during the first collapse of clusters and they might play an important role in driving the observed environmental dependence of galaxy properties at z = 2.15.

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Section: Discussionmentioning

confidence: 99%

The environmental dependence of galaxy properties atz = 2

Tanaka¹,

Breuck²,

Venemans³

et al. 2010

A&A

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show abstract

“…The GAMA survey (Driver et al 2011;Hopkins et al 2013) is a large multi-wavelength study of galaxy formation and evolution using the multi-object 2-degree Field (2dF) robotic fibre positioner, coupled with the AAOmega spectrograph (Sharp et al 2006) on the Anglo-Australian Telescope (AAT). 2dF has 392 fibres (and 8 guide fibres), each with a diameter of 2 arcsec on the sky (corresponding to ∼ 9 kpc at z=0.3).…”

Section: The Gama Surveymentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): the environments of high- and low-excitation radio galaxies

Ching

Croom

Sadler

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We study the environments of low-and high-excitation radio galaxies (LERGs and HERGs respectively) in the redshift range 0.01 < z < 0.4, using a sample of 399 radio galaxies and environmental measurements from the Galaxy And Mass Assembly (GAMA) survey. In our analysis we use the fifth nearest neighbour density (Σ 5 ) and the GAMA galaxy groups catalogue (G3Cv6) and construct control samples of galaxies matched in stellar mass and colour to the radio-detected sample.We find that LERGs and HERGs exist in different environments and that this difference is dependent on radio luminosity. High-luminosity LERGs (L NVSS 10 24 W Hz −1 ) lie in much denser environments than a matched radio-quiet control sample (about three times as dense, as measured by Σ 5 ), and are more likely to be members of galaxy groups (82 +5 −7 percent of LERGs are in GAMA groups, compared to 58 +3 −3 percent of the control sample). In contrast, the environments of the HERGs and lower luminosity LERGs are indistinguishable from that of a matched control sample. Our results imply that high-luminosity LERGs lie in more massive haloes than non-radio galaxies of similar stellar mass and colour, in agreement with earlier studies (Wake et al. 2008;Donoso et al. 2010). When we control for the preference of LERGs to be found in groups, both high-and low-luminosity LERGs are found in higher-mass haloes (∼ 0.2 dex; at least 97 percent significant) than the non-radio control sample.

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“…Despite the ability of integral field spectroscopy to sample a large area of a target source, we are often unable to observe Hα emission in the outer regions of galaxies. A correction for this aperture bias has been developed by Hopkins et al (2003) and Brinchmann et al (2004) for single fibre spectroscopic observations of galaxies but an analogous correction has not been applied to this data (but see Richards et al 2016, for a discussion of aperture corrections to star formation rates with SAMI). There is no systematic correlation between the projected sizes of the galaxies in our sample and other galaxy properties including M * and Σ5, meaning that aperture effects will not have a strong impact on the integrated specific star formation rates we present here.…”

Section: Binning and The Balmer Decrementmentioning

confidence: 99%

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Schaefer

Croom

Allen

et al. 2016

Mon. Not. R. Astron. Soc.

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We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph (SAMI) Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially-resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of Hα emission we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M * ; 10 8.1 -10 10.95 M ) and in 5 th nearest neighbour local environment density (Σ 5 ; 10 −1.3 -10 2.1 Mpc −2 ). We show that star formation rate gradients in galaxies are steeper in dense (log 10 (Σ 5 /Mpc 2 ) > 0.5) environments by 0.58 ± 0.29 dex r e −1 in galaxies with stellar masses in the range 10 10 < M * /M < 10 11 and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density the star-formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scaleradius ratio (r 50,Hα /r 50,cont ), which compares the extent of ongoing star formation to previous star formation. With this metric we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from ∼ 5 ± 4% in low-density environments (log 10 (Σ 5 /Mpc 2 ) < 0.0) to 30 ± 15% in the highest density environments (log 10 (Σ 5 /Mpc 2 ) > 1.0). These lines of evidence strongly suggest that with increasing local environment density the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.

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Star Formation Rate Indicators in the Sloan Digital Sky Survey

Cited by 356 publications

References 65 publications

The environmental dependence of galaxy properties atz = 2

The environmental dependence of galaxy properties atz = 2

Galaxy And Mass Assembly (GAMA): the environments of high- and low-excitation radio galaxies

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

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