Toward a Resolution of the Discrepancy between Different Estimators of Star Formation Rate

Hopkins, A. M.; Connolly, A. J.; Haarsma, D. B.; Cram, L. E.

doi:10.1086/321113

Cited by 214 publications

(346 citation statements)

References 40 publications

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“…From their measurements, Domínguez et al (2013) report an increase in the optical depth with increasing observed luminosity. A similar trend is also reported by Hopkins et al (2001) and Sobral et al (2012). However, the GALACTICUS optical depths for all three dust methods are consistent with no correlation between optical depth and observed luminosity.…”

Section: Comparison To Wisp Optical Depthssupporting

confidence: 88%

Predicting Hα emission-line galaxy counts for future galaxy redshift surveys

Merson

Wang

Benson

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Knowledge of the number density of Hα emitting galaxies is vital for assessing the scientific impact of the Euclid and WFIRST missions. In this work we present predictions from a galaxy formation model, GALACTICUS, for the cumulative number counts of Hα-emitting galaxies. We couple GALACTICUS to three different dust attenuation methods and examine the counts using each method. A χ 2 minimisation approach is used to compare the model predictions to observed galaxy counts and calibrate the dust parameters. We find that weak dust attenuation is required for the GALACTICUS counts to be broadly consistent with the observations, though the optimum dust parameters return large values for χ 2 , suggesting that further calibration of GALACTICUS is necessary. The model predictions are also consistent with observed estimates for the optical depth and the Hα luminosity function. Finally we present forecasts for the redshift distributions and number counts for two Euclid-like and one WFIRST-like survey. For a Euclid-like survey with redshift range 0.9 z 1.8 and Hα + [NII] blended flux limit of 2 × 10 −16 erg s −1 cm −2 we predict a number density between 3900-4800 galaxies per square degree. For a WFIRST-like survey with redshift range 1 z 2 and blended flux limit of 1 × 10 −16 erg s −1 cm −2 we predict a number density between 10400-15200 galaxies per square degree.

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Section: Comparison To Wisp Optical Depthssupporting

confidence: 88%

Predicting Hα emission-line galaxy counts for future galaxy redshift surveys

Merson

Wang

Benson

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The first part of the correlation between the dust extinction and the luminosity of the galaxies has already been reported (e.g. Wang & Heckman 1996, Buat et al 1999) and can probably explain the present results without invoking an extra link between the extinction and the star formation rate as suggested by Hopkins et al (2001).…”

Section: The Extinction In the Hα Emission Linesupporting

confidence: 75%

“…Only spatially resolved studies would allow to remove this uncertainty. Hopkins et al (2001) and Sullivan et al (2001) report a positive correlation between the dust extinction traced by the Balmer decrement and the star formation rate of the galaxies traced by their total FIR or Hα luminosities. In Fig.…”

Section: The Extinction In the Hα Emission Linementioning

confidence: 97%

Star Formation and Dust Extinction in Nearby Star Forming and Starburst Galaxies

Buat

Boselli²,

Gavazzi³

et al. 2002

The Evolution of Galaxies

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Abstract. We study the star formation rate and dust extinction properties of a sample of nearby star forming galaxies as derived from Hα and UV (∼ 2000Å) observations and we compare them to those of a sample of starburst galaxies. The dust extinction in Hα is estimated from the Balmer decrement and the extinction in UV using the FIR to UV flux ratio or the attenuation law for starburst galaxies of Calzetti et al. (2000). The Hα and UV emissions are strongly correlated with a very low scatter for the star forming objects and with a much higher scatter for the starburst galaxies. The Hα to UV flux ratio is found larger by a factor ∼ 2 for the starburst galaxies. We compare both samples with a purely UV selected sample of galaxies and we conclude that the mean Hα and UV properties of nearby star forming galaxies are more representative of UV selected galaxies than starburst galaxies. We emphasize that the Hα to UV flux ratio is strongly dependent on the dust extinction: the positive correlation found between FHα/FUV and FFIR/FUV vanishes when the Hα and UV flux are corrected for dust extinction. The Hα to UV flux ratios converted into star formation rate and combined with the Balmer decrement measurements are tentatively used to estimate the dust extinction in UV.

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“…Hopkins et al (2001) and Sullivan et al (2001) report an increase of the F(H )/F(H ) ratio, used to measure extinction, with the SFR of galaxies. They suggest to use the fit to this correlation in order to account for dust extinction when H is not available.…”

Section: Introductionmentioning

confidence: 99%

A Multiwavelength Approach to the Star Formation Rate Estimation in Galaxies at Intermediate Redshifts

Cardiel

Elbaz

Schiavon

et al. 2003

ApJ

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We use a sample of seven starburst galaxies at intermediate redshifts (z $ 0:4 and 0.8) with observations ranging from the observed ultraviolet to 1.4 GHz, to compare the star formation rate (SFR) estimators that are used in the different wavelength regimes. We find that extinction-corrected H underestimates the SFR, and the degree of this underestimation increases with the infrared luminosity of the galaxies. Galaxies with very different levels of dust extinction as measured with SFR IR /SFR(H , uncorrected for extinction) present a similar attenuation A[H ], as if the Balmer lines probed a different region of the galaxy than the one responsible for the bulk of the IR luminosity for large SFRs. In addition, SFR estimates derived from [O ii] 3727 match very well those inferred from H after applying the metallicity correction derived from local galaxies. SFRs estimated from the UV luminosities show a dichotomic behavior, similar to that previously reported by other authors in galaxies at zd0:4. Here we extend this result up to z $ 0:8. Finally, one of the studied objects is a luminous compact galaxy (LCG) that may be suffering similar dust-enshrouded star formation episodes. These results highlight the relevance of quantifying the actual L IR of LCGs, as well as that of a much larger and generic sample of luminous infrared galaxies, which will be possible after the launch of SIRTF.

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Toward a Resolution of the Discrepancy between Different Estimators of Star Formation Rate

Cited by 214 publications

References 40 publications

Predicting Hα emission-line galaxy counts for future galaxy redshift surveys

Predicting Hα emission-line galaxy counts for future galaxy redshift surveys

Star Formation and Dust Extinction in Nearby Star Forming and Starburst Galaxies

A Multiwavelength Approach to the Star Formation Rate Estimation in Galaxies at Intermediate Redshifts

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