Optical and infrared diagnostics of SDSS galaxies in the SWIRE survey

Davoodi, Payam; Pozzi, F.; Oliver, Seb; Polletta, M.; Afonso-Luis, A.; Farrah, D.; Hatziminaoglou, E.; Rodighiero, G.; Berta, S.; Waddington, I.; Lonsdale, C. J.; Rowan-Robinson, M.; Shupe, D. L.; Evans, T. M.; Fan, Fang; Smith, H. E.; Surace, J.

doi:10.1111/j.1365-2966.2006.10793.x

Cited by 24 publications

(35 citation statements)

References 89 publications

(116 reference statements)

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“…2) which are spectroscopically classed as star forming varies with both environment and luminosity. Globally, we find that 31 per cent of red‐sequence galaxies (with M r < −17) are star forming, similar to that found by Wolf et al (2005), but larger than the 17 per cent obtained by Davoodi et al (2006). This difference is most likely due to their sample being biased towards more luminous galaxies than ours, and indeed we find just 18 per cent of M r < −20 galaxies to be star forming.…”

Section: The Make‐up Of the Red Sequence In Optical Surveyssupporting

confidence: 76%

“…Hence, while passive galaxies are red, red galaxies are not necessarily passive. In particular, Davoodi et al (2006) find that 17 per cent of red‐sequence galaxies are dusty, star‐forming galaxies (identified by their high 24/3.6 μm flux ratios and Hα emission), while Wolf, Gray & Meisenheimer (2005) find that dusty, star‐forming galaxies make‐up more than one‐third of the red‐sequence population, finding them preferentially in the outskirts of clusters. Given that the relative fractions of passively evolving/red and star‐forming/blue galaxies of a given luminosity are strongly dependent on local environment, particularly at the faint end (Balogh et al 2004; Baldry et al 2006; Paper II), the contamination of the red sequence by star‐forming galaxies is also likely to be strongly dependent on environment.…”

Section: The Make‐up Of the Red Sequence In Optical Surveysmentioning

confidence: 99%

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The SDSS-GALEX viewpoint of the truncated red sequence in field environments at z ∼ 0

Haines¹,

Gargiulo²,

Merluzzi³

2008

Monthly Notices RAS

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We combine Galaxy Evolution ExplorerGALEX near‐ultraviolet (NUV) photometry with a volume‐limited sample of local (0.005 < z < 0.037) Sloan Digital Sky Survey (SDSS) DR4 galaxies to examine the composition and the environmental dependencies of the optical and ultraviolet (UV)‐optical colour–magnitude (CM) diagrams. We find that ∼30 per cent of red‐sequence galaxies in the optical CM diagram show signs of ongoing star formation from their spectra having EW(Hα) > 2 Å. This contamination is greatest at faint magnitudes (Mr > −19) and in field regions where as many as three‐quarters of red‐sequence galaxies are star forming, and as such has important consequences for following the build‐up of the red sequence. The NUV −r colour instead allows a much more robust separation of passively evolving and star‐forming galaxies, which allows the build‐up of the UV‐selected red sequence with redshift and environment to be directly interpreted in terms of the assembly of stellar mass in passively evolving galaxies. In isolated field regions, the number density of UV‐optical red‐sequence galaxies declines rapidly at magnitudes fainter than Mr∼−19 and appears completely truncated at Mr∼−18. These results support the downsizing paradigm whereby the red sequence is assembled from the top down, being already largely in place at the bright end by z∼ 1, and the faint end filled in at later epochs in clusters and groups through environment‐related processes such as ram‐pressure stripping or galaxy harassment.

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Section: The Make‐up Of the Red Sequence In Optical Surveyssupporting

confidence: 76%

Section: The Make‐up Of the Red Sequence In Optical Surveysmentioning

confidence: 99%

The SDSS-GALEX viewpoint of the truncated red sequence in field environments at z ∼ 0

Haines¹,

Gargiulo²,

Merluzzi³

2008

Monthly Notices RAS

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“…The luminosity of the 3.6 m band is often treated as a tracer of the stellar component (Wu et al 2005a;Davoodi et al 2006;etc. ), as well as a test of the validity of the mass determination ( Hancock et al 2007).…”

Section: Estimation Of the Stellar Massmentioning

confidence: 99%

Morphological Dependence of Mid-Infrared Properties of SDSS Galaxies in theSpitzerSWIRE Survey

Cao

et al. 2007

Astron J

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We explore the correlation between morphological types and mid-infrared (MIR) properties of an optically fluxlimited sample of 154 galaxies from the Fourth Data Release ( DR4) of the Sloan Digital Sky Survey (SDSS), crosscorrelated with Spitzer SWIRE fields of ELAIS-N1, ELAIS-N2, and the Lockman Hole. Aperture photometry is performed on the SDSS and Spitzer images to obtain optical and MIR properties. The morphological classifications are given based on both visual inspection and bulge-disk decomposition in SDSS g-and r-band images. The average bulge-to-total ratio (B/T ) is a smooth function over different morphological types. Both the 8 m (dust) and 24 m (dust) luminosities and their relative luminosity ratios to 3.6 m (MIR dust-to-star ratios) present obvious correlations with both the Hubble T-type and B/T . The early-type galaxies notably differ from the late types in the MIR properties, especially in the MIR dust-to-star ratios. It is suggested that the MIR dust-to-star ratio of either L ½8 m (dust)/L ½3:6 m or L ½24 m (dust)/L ½3:6 m is an effective way to separate the early-type galaxies from the late-type ones. Based on the tight correlation between the stellar mass and the 3.6 m luminosity, we have derived a formula to calculate the stellar mass from the latter. We have also investigated the MIR properties of both edge-on galaxies and barred galaxies in our sample. Since they present similar MIR properties to the other sample galaxies, they do not influence the MIR properties obtained for the entire sample.

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“…Numerous studies have determined the stellar mass of galaxies by using near-infrared observations (Bundy et al 2005;Davoodi et al 2006) or spectral synthesis fitting to optical spectra (Kauffmann et al 2003;Tremonti et al 2004). Generally, the mass of a galaxy is in an approximate range from 10 9 to 10 12 M .…”

Section: Introductionmentioning

confidence: 99%

Investigating merging galaxies by using Pan-STARRS images

Lin¹,

Yu²,

Huang³

et al. 2017

A&A

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Aims. We studied the r -, z -, and y -band images of merging galaxies from the observations of the Panoramic Survey Telescope & Rapid Response System (Pan-STARRS). The merging galaxies were selected from our merging catalog that was created by checking the images of the Red-Sequence Cluster Survey 2 from the observations of the Canada France Hawaii Telescope. Methods. By using the homomorphic-aperture, we determined the photometric results of these merging systems. To obtain accurate photometry, we calibrated the Pan-STARRS r -, z -, and y -band data to match the results of Sloan Digital Sky Survey Data Release 9. We also investigated the stellar masses of the merging galaxies by comparing the Wide-field Infrared Survey Explorer 3.4 µm emission with the calibrated y -band data.Results. We present a catalog of the r -, z -, and y -band photometric results for 4698 merging galaxies. For extended sources, our results suggest that the homomorphic-aperture method can obtain more reasonable results than the Desktop Virtual Observatory photometry. We derived new relations between the Pan-STARRS y -band luminosities and the stellar masses of the merging galaxies. Our results show that the stellar masses of the merging galaxies range from 10 8 to 10 13 M ; some of the dry mergers could be as massive as 10 13 M .

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Optical and infrared diagnostics of SDSS galaxies in the SWIRE survey

Cited by 24 publications

References 89 publications

The SDSS-GALEX viewpoint of the truncated red sequence in field environments at z ∼ 0

The SDSS-GALEX viewpoint of the truncated red sequence in field environments at z ∼ 0

Morphological Dependence of Mid-Infrared Properties of SDSS Galaxies in theSpitzerSWIRE Survey

Investigating merging galaxies by using Pan-STARRS images

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