Metallicity dependent calibrations of flux based SFR tracers

Bicker, Jens; Alvensleben, U. Fritze–v.

doi:10.1051/0004-6361:200500194

Cited by 31 publications

(30 citation statements)

References 26 publications

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“…The idea was to calibrate the [Oii]λ3727/Hα emission-line ratio versus the metallicity, and then to use it to recover the SFR from the Hα luminosity, itself derived from the [Oii]λ3727 luminosity. The dependence on the metallicity of the [Oii]λ3727/Hα emission-line ratio, or more generally the [Oii]λ3727 based SFR calibrations, has been later confirmed by Mouhcine et al (2005) and Bicker & Fritze-v. Alvensleben (2005).…”

Section: Article Published By Edp Sciencesmentioning

confidence: 82%

Emission-lines calibrations of the star formation rate from the Sloan Digital Sky Survey

Argence

Lamareille²

2009

A&A

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Aims. Up to now, the study of the star formation rate in galaxies has been based mainly on the Hα emission-line luminosity. However, this standard calibration cannot be applied at all redshifts if there is only one instrumental setup. Surveys based on optical spectroscopy do not observe the Hα emission line at redshifts higher than z ∼ 0.5. Our goal is to study existing star formation rate calibrations and to provide new ones, still based on emission-line luminosities, which can be applied for various instrumental setups. Methods. We used the SDSS public data release DR4, which gives star formation rates and emission-line luminosities for more than 100 000 starforming galaxies observed at low redshifts. We take advantage of this statistically significant sample in order to study the relations, based on these data, between the star formation rate and the luminosities of some well-chosen emission lines. We correct the emission-line measurements for dust attenuation using the same attenuation curve as the one used to derive the star formation rates. Results. We confirm that the best results are obtained when relating star formation rates to the Hα emission-line luminosity, itself corrected for dust attenuation. This calibration has an uncertainty of 0.17 dex. We show that one has to carefully check the method used to derive the dust attenuation and to use the adequate calibration: in some cases, the standard scaling law has to be replaced by a more general power law. When data are corrected for dust attenuation but the Hα emission line not observed, the use of the Hβ emission line, if possible, has to be preferred to the [Oii]λ3727 emission line. In the case of uncorrected data, the correction for dust attenuation can be assumed as a constant mean value, but we show that such a method leads to poor results in terms of dispersion and residual slope. Self-consistent corrections, such as previous studies based on the absolute magnitude, give better results in terms of dispersion but still suffer from systematic shifts and/or residual slopes. The best results with data not corrected for dust attenuation are obtained when using the observed [Oii]λ3727 and Hβ emission lines together. This calibration has an uncertainty of 0.23 dex.

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Section: Article Published By Edp Sciencesmentioning

confidence: 82%

Emission-lines calibrations of the star formation rate from the Sloan Digital Sky Survey

Argence

Lamareille²

2009

A&A

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“…Another possible remaining issue is a metallicity dependence of the Hα luminosity (e.g., Bicker & Fritze-v. Alvensleben 2005;Dopita et al 2006). A lower stellar metallicity would result in a higher stellar temperature, thus the larger number of ionizing photons.…”

Section: Discussionmentioning

confidence: 99%

ENHANCED STAR FORMATION OF LESS MASSIVE GALAXIES IN A PROTOCLUSTER AT z = 2.5

Hayashi¹,

Kodama

Tanaka³

et al. 2016

ApJL

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We investigate a correlation between star formation rate (SFR) and stellar mass for Hα emission-line galaxies (HAEs) in one of the richest protoclusters ever known at z∼2.5, the USS1558-003 protocluster. This study is based on a 9.7 hr narrowband imaging data with MOIRCS on the Subaru telescope. We are able to construct a sample in combination with additional H-band data taken with WFC3 on the Hubble Space Telescope, of 100 HAEs reaching the dust-corrected SFRs down to 3 M e yr −1 and the stellar masses down to 10 8.0 M e . We find that while the star-forming galaxies with 10 9.3 M e are located on the universal SFR-mass main sequence (MS) irrespective of the environment, less massive star-forming galaxies with 109.3 M e show a significant upward scatter from the MS in this protocluster. This suggests that some less massive galaxies are in a starburst phase, although we do not know yet if this is due to environmental effects.

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“…Luminosities in a wide variety of filter systems and colors are obtained by folding the spectra with the respective filter response functions. In Anders & Fritze-v. Alvensleben (2002) we added the emission contributions from gas ionized by young stars both in terms of continuous and line emission for the respective metallicities to our single burst single metallicity models, while in Bicker & Fritze-v. Alvensleben (2005) we discussed its effects in the context of galaxies.…”

Section: Undisturbed Galaxiesmentioning

confidence: 99%

“…Bicker & Fritze-v. Alvensleben 2005). It has been shown to have a large impact, even on broad band luminosities and colors, during strong starbursts by Krüger et al (1995) (see also Anders & Fritze-v. Alvensleben 2003).…”

Section: Undisturbed Galaxiesmentioning

confidence: 99%

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

Alvensleben¹,

Bicker

2006

A&A

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We present evolutionary synthesis models for galaxies of spectral types Sa through Sd with starbursts of various strengths triggered at various redshifts and study their photometric evolution before, during, and after their bursts in a cosmological context. We find that bursts at high redshift, even very strong ones, only cause a small blueing of their intrinsically blue young parent galaxies. At lower redshift, in contrast, even small bursts cause a significant blueing of their intrinsically redder galaxies. While the burst phase is generally short, typically a few hundred Myr in normal-mass galaxies, the postburst stage with its red colors and, in particular the very red ones for early bursts at high redshift, lasts much longer, on the order of several Gyr. We find that, even without any dust, which in the postburst stage is not expected to play an important role anyway, models easily reach the colors of EROs in the redshift range z ∼ 2 through z ∼ 0.5 after starbursts at redshifts between 2 and 4. We therefore propose a third alternative for the ERO galaxies beyond the two established ones of passive galaxies vs. dusty starbursts: the dust-free post-(strong-)starbursts. A very first comparison of our models to HDF data with photometric redshifts shows that almost all of the outliers that could not be described with our chemically consistent models for undisturbed normal galaxy types E through Sd can now be explained very well. Galaxies in the redshift range from z ∼ 2.5 to z ∼ 0.5 that are redder, and in some cases much redder, than our reddest undisturbed model for a high-metallicity classical elliptical are well described by post-starburst models after starbursts at redshifts between 2 and 4. Galaxies bluer than our bluest low metallicity Sd model, most of which have redshifts lower than 1, are well explained by ongoing starbursts.

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Metallicity dependent calibrations of flux based SFR tracers

Cited by 31 publications

References 26 publications

Emission-lines calibrations of the star formation rate from the Sloan Digital Sky Survey

Emission-lines calibrations of the star formation rate from the Sloan Digital Sky Survey

ENHANCED STAR FORMATION OF LESS MASSIVE GALAXIES IN A PROTOCLUSTER AT z = 2.5

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

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