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

Cardiel, N.; Elbaz, D.; Schiavon, Ricardo P.; Willmer, Christopher N. A.; Koo, David C.; Phillips, Andrew C.; Gallego, J.

doi:10.1086/345594

Cited by 43 publications

(42 citation statements)

References 103 publications

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“…To correct for redshift effects, we adopt a steep nonthermal radio spectrum whose flux obeys a power law of the form n Ϫa (Cardiel et al 2003) and has a spectral index of a p 0.8 (Condon 1992) and compute rest-frame radio luminosities at 1.4 GHz.…”

Section: Mir Luminosities and Correlation Analysismentioning

confidence: 99%

PAH and Mid-Infrared Luminosities as Measures of Star Formation Rate in Sp i t zer First Look Survey Galaxies

Cao

Hao

et al. 2005

ApJ

209

174

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We present evidence that the 8 mm (dust) and 24 mm luminosities of star-forming galaxies are both strongly correlated with their 1.4 GHz and Ha luminosities over a range in luminosity of 2-3 orders of magnitude. At the bright end, the correlations are found to be essentially linear over a luminosity range of about 2 orders of magnitude (corresponding to star formation rates of several tenths to several tens of solar masses per year). However, at the faint end there appears to be a slope change for dwarf galaxies, possibly due to the lower dustto-gas ratios and lower metallicities of the dwarfs. The correlations suggest that PAH features and mid-IR continuum emissions are good measures of the star formation rates of galaxies, and we present calibrations of star formation rates based on existing radio and Ha relations. Our findings are based on a sample of star-forming galaxies selected from the main field of the Spitzer First Look Survey with the aid of spectroscopic data from the Sloan Digital Sky Survey and VLA 1.4 GHz data.

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Section: Mir Luminosities and Correlation Analysismentioning

confidence: 99%

PAH and Mid-Infrared Luminosities as Measures of Star Formation Rate in Sp i t zer First Look Survey Galaxies

Cao

Hao

et al. 2005

ApJ

209

174

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“…Note that the 60 m flux densities were used for this purpose because they have the fewest upper limits. Lawrence et al (1989) and Cardiel et al (2003) gave, respectively,…”

Section: Accretion Rates and Star Formation Ratesmentioning

confidence: 99%

The Physical Connections among Infrared QSOs, Palomar‐Green QSOs, and Narrow‐Line Seyfert 1 Galaxies

Hao

Xia

Mao

et al. 2005

ApJ

110

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We study the properties of infrared-selected QSOs (IR QSOs), optically selected Palomar-Green QSOs (PG QSOs), and narrow-line Seyfert 1 galaxies (NLS1s). We compare their properties from the IR to the optical and examine various correlations among the black hole mass, accretion rate, star formation rate, and optical and IR luminosities. We find that the IR excess in IR QSOs is mostly in the far-IR, and their IR spectral indices suggest that the excess emission is from low-temperature dust heated by starbursts rather than active galactic nuclei (AGNs). The IR excess is therefore a useful criterion to separate the relative contributions of starbursts and AGNs. We further find a tight correlation between the star formation rate and the accretion rate of central AGNs for IR QSOs. The ratio of the star formation rate and the accretion rate is about several hundred for IR QSOs but decreases with the central black hole mass. This shows that the tight correlation between the stellar mass and the central black hole mass is preserved in massive starbursts during violent mergers. We suggest that the higher Eddington ratios of NLS1s and IR QSOs imply that they are in the early stage of evolution toward classical Seyfert 1 galaxies and QSOs, respectively.

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“…Therefore the vast bulk of the star formation is missed when the [O ] line emission is used. A large fraction of the star formation in Cl 0024+1654 is enshrouded by dust (see Cardiel et al 2003 for a thorough discussion on the comparison of SFRestimators). Duc et al (2002) and Balogh et al (2002) have arrived at a very similar conclusion for the cluster Abell 1689, which has many mid-infrared sources.…”

Section: The Ratios Of Sfr[ir]/sfr[o ]mentioning

confidence: 99%

An ISOCAM survey through gravitationally lensing galaxy clusters

Metcalfe

Kneib²,

McBreen³

et al. 2005

A&A

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Abstract.Observations of the core of the massive cluster Cl 0024+1654, at a redshift z ∼ 0.39, were obtained with the Infrared Space Observatory using ISOCAM at 6.7 µm (hereafter 7 µm) and 14.3 µm (hereafter 15 µm). Thirty five sources were detected at 15 µm and thirteen of them are spectroscopically identified with cluster galaxies. The remaining sources consist of four stars, one quasar, one foreground galaxy, three background galaxies and thirteen sources with unknown redshift. The sources with unknown redshift are all likely to be background sources that are gravitationally lensed by the cluster. The spectral energy distributions (SEDs) of twelve cluster galaxies were fit from a selection of 20 models using the program GRASIL. The ISOCAM sources have best-fit SEDs typical of spiral or starburst models observed 1 Gyr after the main starburst event. The star formation rates were obtained for cluster members. The median infrared luminosity of the twelve cluster galaxies is ∼1.0 × 10 11 L , with 10 having infrared luminosity above 9 × 10 10 L , and so lying near or above the 1 × 10 11 L threshold for identification as a luminous infrared galaxy (LIRG). The [O ] star formation rates obtained for 3 cluster galaxies are one to two orders of magnitude lower than the infrared values, implying that most of the star formation is missed in the optical because it is enshrouded by dust in the starburst galaxy. The cluster galaxies in general are spatially more concentrated than those detected at 15 µm. However the velocity distributions of the two categories are comparable. The colour−magnitude diagramme is given for the galaxies within the ISOCAM map. Only 20% of the galaxies that are significantly bluer than the cluster main sequence were detected at 15 µm, to the limiting sensitivity recorded. The counterparts of about half of the 15 µm cluster sources are blue, luminous, star-forming systems and the type of galaxy that is usually associated with the Butcher-Oemler effect. HST images of these galaxies reveal a disturbed morphology with a tendency for an absence of nearby companions. Surprisingly the counterparts of the remaining 15 µm cluster galaxies lie on the main sequence of the colour-magnitude diagramme. However in HST images they all have nearby companions and appear to be involved in interactions and mergers. Dust obscuration may be a major cause of the 15 µm sources appearing on the cluster main sequence. The majority of the ISOCAM sources in the Butcher-Oemler region of the colourmagnitude diagram are best fit by spiral-type SEDs whereas post-starburst models are preferred on the main sequence, with the starburst event probably triggered by interaction with one or more galaxies. Finally, the mid-infrared results on Cl 0024+1654 are compared with four other clusters observed with ISOCAM. Scaling the LIRG count in Cl 0024+1654 to the clusters Abell 370, Abell 1689, Abell 2218 and Abell 2390 with reference to their virial radii, masses, distances, and the sky area scanned in each case, we compared the number o...

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

Cited by 43 publications

References 103 publications

PAH and Mid-Infrared Luminosities as Measures of Star Formation Rate in Sp i t zer First Look Survey Galaxies

PAH and Mid-Infrared Luminosities as Measures of Star Formation Rate in Sp i t zer First Look Survey Galaxies

The Physical Connections among Infrared QSOs, Palomar‐Green QSOs, and Narrow‐Line Seyfert 1 Galaxies

An ISOCAM survey through gravitationally lensing galaxy clusters

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