Star formation rates of distant luminous infrared
 galaxies derived from H<i>α</i> and IR 
 luminosities

Flores, H.; Hammer, F.; Elbaz, D.; Césarsky, C. J.; Liang, Y. C.; Fadda, D.; Gruel, N.

doi:10.1051/0004-6361:20034491

Cited by 61 publications

(69 citation statements)

References 15 publications

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“…(A color version of this figure is available in the online journal.) (e.g., Flores et al 2004;Liang et al 2004;Rodrigues et al 2008;Villar et al 2008;Savaglio et al 2005). However, the majority of such studies have targeted LIRGs and ULIRGs.…”

Section: Comparison With Other Extinction Relationsmentioning

confidence: 99%

NEBULAR ATTENUATION IN Hα-SELECTED STAR-FORMING GALAXIES ATz= 0.8 FROM THE NewHα SURVEY

Momcheva

Lee

et al. 2013

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We present measurements of the dust attenuation of Hα-selected emission-line galaxies at z = 0.8 from the NewHα narrowband survey. The analysis is based on deep follow-up spectroscopy with Magellan/IMACS, which captures the strong rest-frame optical emission lines fromThe spectroscopic sample used in this analysis consists of 341 confirmed Hα emitters. We place constraints on the active galactic nucleus (AGN) fraction using diagnostics that can be applied at intermediate redshift. We find that at least 5% of the objects in our spectroscopic sample can be classified as AGNs and 2% are composite, i.e., powered by a combination of star formation and AGN activity. We measure the dust attenuation for individual objects from the ratios of the higher order Balmer lines. The Hβ and Hγ pair of lines is detected with S/N > 5 in 55 individual objects and the Hβ and Hδ pair is detected in 50 individual objects. We also create stacked spectra to probe the attenuation in objects without individual detections. The median attenuation at Hα based on the objects with individually detected lines is A(Hα) = 0.9 ± 1.0 mag, in good agreement with the attenuation found in local samples of star-forming galaxies. We find that the z = 0.8 galaxies occupy a similar locus of attenuation as a function of magnitude, mass, and star formation rate (SFR) as a comparison sample drawn from the SDSS DR4. Both the results from the individual z = 0.8 galaxies and from the stacked spectra show consistency with the mass-attenuation and SFR-attenuation relations found in the local universe, indicating that these relations are also applicable at intermediate redshift.

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Section: Comparison With Other Extinction Relationsmentioning

confidence: 99%

NEBULAR ATTENUATION IN Hα-SELECTED STAR-FORMING GALAXIES ATz= 0.8 FROM THE NewHα SURVEY

Momcheva

Lee

et al. 2013

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“…If unrealistic values of A V (≥3.5) are taken to calculate the SFRs of these galaxies, hence the SF density, this could lead to severe overestimations. Recall that for the luminous infrared galaxies, Flores et al (2004a) never find A V values larger than 3.5. And the average color excesses, E(B−V), of luminous infrared galaxies (LIGs) studied by Veilleux et al (1995) are only 0.72, 0.99 and 1.14 in Seyfert 2, H II LIGs and LINERs, respectively.…”

Section: Estimates Of Cosmic Star Formation Density (Csfd)mentioning

confidence: 99%

Misleading results from low-resolution spectroscopy: From galaxy interstellar medium chemistry to cosmic star formation density

Liang

Hammer

Flores

et al. 2004

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Abstract. Low resolution spectroscopy (R = 150) from the Canada-France-Redshift Survey (CFRS) revealed intriguing properties for low redshift galaxies (z ≤ 0.3): nearly half of their spectra show prominent Hα emission lines, but no Hβ emission line and barely detected [O ] λ3727, and [O ] λ5007 lines. We call these objects "CFRS Hα-single" galaxies and have reobserved a subsample of them at higher spectral resolution, associated with a subsample of more normal emission line galaxies. Good S/N spectroscopy at the VLT and the CFHT, with moderate spectral resolution (R > 600), have allowed us to perform a full diagnostic of their interstellar medium chemistry. "CFRS Hα-single" galaxies and most of the star forming spirals have high extinctions (A V > 2), high stellar masses and over-solar oxygen abundances. From the present study, we find it hazardous to derive the detailed properties of galaxies (gas chemical abundances, interstellar extinction, stellar population, star formation rates and history) using spectra with resolutions below 600. One major drawback is indeed the estimated extinction which requires a proper analysis of the underlying Balmer absorption lines. We find that, with low resolution spectroscopy, star formation rates (SFRs) can be either underestimated or overestimated by factors reaching 10 (average 3.1), even if one accounts for ad hoc extinction corrections. These effects are prominent for a large fraction of evolved massive galaxies especially those experiencing successive bursts (A and F stars dominating their absorption spectra). Further estimates of the cosmic star formation density at all redshifts mandatorily requires moderate resolution spectroscopy to avoid severe and uncontrolled biases.

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“…However, the consistent derivation of the signal-to-noise (S /N) ratio on the intrinsic luminosities lead to large uncertainties on the measured visual attenuation. Moreover, there is evidence of some completely obscured star formation as found in the most luminous objects studied in Flores et al (2004) or in Cardiel et al (2003). The limited statistics of those studies clearly call for an extention of the sample of distant LIRGs, with good S /N on the optical continuum and high spectral resolution, to robustly determine which fraction of the star formation taking place in LIRGs and ULIRGs is completely obscured by dust.…”

Section: Introductionmentioning

confidence: 99%

The star formation history of luminous infrared galaxies

Marcillac

Elbaz

Charlot

et al. 2006

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Aims. We constrain the past star formation histories of a sample of 25 distant (z ∼ 0.7) luminous infrared galaxies (LIRGs) detected with the mid infrared cameras ISOCAM and MIPS onboard the ISO and Spitzer satellites. Methods. We used high-resolution VLT-FORS2 spectroscopy in addition to a comprehensive library of 200 000 model optical spectra to derive Bayesian likelihood estimates of the star formation histories of these galaxies, based on analysis of Balmer absorption lines and the 4000 Å break. Results. The locus of distant LIRGs in the diagram defined by Hδ A and D4000 is roughly comparable to that of local LIRGs observed with IRAS, suggesting that no trend toward an evolution is detected between the local and distant LIRGs. We obtain similar results when using either the H8 or the Hδ A Balmer absorption-line indices in combination with D4000. By computing a birthrate parameter (b = SFR/ SFR ) of 4 ± 1, we confirme that the distant LIRGs are currently experiencing a major phase of star formation. The most likely duration of the bursts is 0.10 +0.16−0.06 Gyr, during which the LIRGs produce ∼5-10% of their current stellar mass. No evidence was found for successive starbursts on the scale of a few times 10 7 yr, such as those predicted by some numerical simulations of major mergers. However, the high number density of those galaxies suggests that they could have experienced between two and four LIRG phases until the present epoch. This scenario is not consistent with the formation of the z ∼ 0.7 LIRGs through the continuous star formation characterizing isolated spiral galaxies as has been independently argued based on their morphology. Instead, minor mergers, tidal interactions, or gas accretion remain plausible triggering mechanisms for more than half of the distant LIRGs that do not harbor the morphology of major mergers.

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Star formation rates of distant luminous infrared galaxies derived from Hα and IR luminosities

Cited by 61 publications

References 15 publications

NEBULAR ATTENUATION IN Hα-SELECTED STAR-FORMING GALAXIES ATz= 0.8 FROM THE NewHα SURVEY

NEBULAR ATTENUATION IN Hα-SELECTED STAR-FORMING GALAXIES ATz= 0.8 FROM THE NewHα SURVEY

Misleading results from low-resolution spectroscopy: From galaxy interstellar medium chemistry to cosmic star formation density

The star formation history of luminous infrared galaxies

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