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Cuillandre, Jean-Charles; Starr, Barry Michael; Isani, Sidik

doi:10.1023/a:1013110613800

Cited by 30 publications

(30 citation statements)

References 1 publication

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“…A detailed summary was provided in Paper I (x 2) as background to computing the DEEP2 luminosity functions; the functions from Paper I ( Tables 3Y5) are adopted here without change. DEEP2 catalogs are derived from Canada-FranceHawaii Telescope (CFHT) images taken with the 12K ; 8K mosaic camera (Cuillandre et al 2001) in B, R, and I in four different regions of the sky. Reduction of the photometric data, object detection, photometric calibration, and construction of the star-galaxy catalogs are described in Coil et al (2004).…”

Section: Deep2mentioning

confidence: 99%

Galaxy Luminosity Functions toz∼1 from DEEP2 and COMBO‐17: Implications for Red Galaxy Formation

Faber

Willmer

Wolf

et al. 2007

ApJ

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981

1,031

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The DEEP2 and COMBO-17 surveys are compared to study luminosity functions of red and blue galaxies to z $ 1. The two surveys have different methods and sensitivities, but nevertheless results agree. After z $ 1, M Ã B has dimmed by 1.2Y1.3 mag for all colors of galaxies, Ã for blue galaxies has hardly changed, and Ã for red galaxies has at least doubled (our formal value is $0.5 dex). Luminosity density j B has fallen by 0.6 dex for blue galaxies but has remained nearly constant for red galaxies. These results imply that the number and total stellar mass of blue galaxies have been substantially constant since z $ 1, whereas those of red galaxies (near L Ã ) have been significantly rising. To explain the new red galaxies, a ''mixed'' scenario is proposed in which star formation in blue cloud galaxies is quenched, causing them to migrate to the red sequence, where they merge further in a small number of stellar mergers. This mixed scenario matches the local boxy-disky transition for nearby ellipticals, as well as red sequence stellar population scaling laws such as the color-magnitude and Mg-relations (which are explained as fossil relics from blue progenitors). Blue galaxies enter the red sequence via different quenching modes, each of which peaks at a different characteristic mass and time. The red sequence therefore likely builds up in different ways at different times and masses, and the concept of a single process that is ''downsizing'' (or upsizing) probably does not apply. Our claim in this paper of a rise in the number of red galaxies applies to galaxies near L Ã . Accurate counts of brighter galaxies on the steep part of the Schechter function require more accurate photometry than is currently available.

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Section: Deep2mentioning

confidence: 99%

Galaxy Luminosity Functions toz∼1 from DEEP2 and COMBO‐17: Implications for Red Galaxy Formation

Faber

Willmer

Wolf

et al. 2007

ApJ

Self Cite

981

1,031

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“…In addition, the field lies at a high (absolute) galactic latitude (l, b) = (172.0, −58.1), resulting in low galactic extinction, and is reasonably far removed from the ecliptic, resulting in acceptable levels of zodiacal light. The field first became the subject of study in 1999 when it was targeted with the Canada-France-Hawai'i 12K wide-field imager (CFH12K; Cuillandre et al 2000) to provide BVRI photometry (McCracken et al 2003;Le Fèvre et al 2004) for the initial phase of the VIMOS VLT Deep Survey (VVDS; Le Fèvre et al 2005) 2 . Shortly thereafter, a subsection of the field was observed in multiple optical bands as part of the deep portion of the CFHTLS providing the basis for numerous future studies.…”

Section: Observations and Reductionmentioning

confidence: 99%

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Lemaux

Floc’h

Fèvre

et al. 2014

A&A

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We investigate of the properties of ∼2000 Herschel/SPIRE far-infrared-selected galaxies from 0 < z < 4 in the CFHTLS-D1 field. Using a combination of extensive spectroscopy from the VVDS and ORELSE surveys, deep multiwavelength imaging from CFHT, VLA, Spitzer, XMM-Newton, and Herschel, and well-calibrated spectral energy distribution fitting, Herschel-bright galaxies are compared to optically-selected galaxies at a variety of redshifts. Herschel-selected galaxies are observed to span a range of stellar masses, colors, and absolute magnitudes equivalent to galaxies undetected in SPIRE. Though many Herschel galaxies appear to be in transition, such galaxies are largely consistent with normal star-forming galaxies when rest-frame colors are utilized. The nature of the star-forming "main sequence" is studied and we warn against adopting this framework unless the main sequence is determined precisely. Herschel galaxies at different total infrared luminosities (L TIR ) are compared. Bluer optical colors, larger nebular extinctions, and larger contributions from younger stellar populations are observed for galaxies with larger L TIR , suggesting that low-L TIR galaxies are undergoing rejuvenated starbursts while galaxies with higher L TIR are forming a larger percentage of their stellar mass. A variety of methods are used to select powerful active galactic nuclei (AGN). Galaxies hosting all types of AGN are observed to be undergoing starbursts more commonly and vigorously than a matched sample of galaxies without powerful AGN and, additionally, the fraction of galaxies with an AGN increases with increasing star formation rate at all redshifts. At all redshifts (0 < z < 4) the most prodigious star-forming galaxies are found to contain the highest fraction of powerful AGN. For redshift bins that allow a comparison (z > 0.5), the highest L TIR galaxies in a given redshift bin are unobserved by SPIRE at subsequently lower redshifts, a trend linked to downsizing. In conjunction with other results, this evidence is used to argue for prevalent AGN-driven quenching in starburst galaxies across cosmic time.

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“…1) in three wide-band Sloan Digital Sky Survey filters : g, r, and z (respectively called F475W, F625W and F850LP on HST). The whole NGC 7023 nebula was observed in August 2002 in the B, V and R filters at the CFHT using the CFH12K CCD mosaic (Cuillandre et al 2001) as part of the CFHT outreach program. A set of 5 dithered exposures of 60 s each were obtained in each filter in order to remove the mosaic gaps and other physical blemishes.…”

Section: Visible Observationsmentioning

confidence: 99%

Extended Red Emission and the evolution of carbonaceous nanograins in NGC 7023

Berné¹,

Joblin²,

Rapacioli

et al. 2008

A&A

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Context. Extended Red Emission (ERE) was recently attributed to the photo-luminescence of either doubly ionized Polycyclic Aromatic Hydrocarbons (PAH ++ ), or charged PAH dimers ([PAH 2 ] + ). Aims. We analysed the visible and mid-infrared (mid-IR) dust emission in the North-West and South photo-dissociation regions of the reflection nebula NGC 7023. Methods. Using a blind signal separation method, we extracted the map of ERE from images obtained with the Hubble Space Telescope, and at the Canada France Hawaii Telescope. We compared the extracted ERE image to the distribution maps of the mid-IR emission of Very Small Grains (VSGs), neutral and ionized PAHs (PAH 0 and PAH + ) obtained with the Spitzer Space Telescope and the Infrared Space Observatory. Results. ERE is dominant in transition regions where VSGs are being photo-evaporated to form free PAH molecules, and is not observed in regions dominated by PAH + . Its carrier makes a minor contribution to the mid-IR emission spectrum. Conclusions. These results suggest that the ERE carrier is a transition species formed during the destruction of VSGs. [PAH 2 ] + appear as good candidates but PAH ++ molecules seem to be excluded.

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Cited by 30 publications

References 1 publication

Galaxy Luminosity Functions toz∼1 from DEEP2 and COMBO‐17: Implications for Red Galaxy Formation

Galaxy Luminosity Functions toz∼1 from DEEP2 and COMBO‐17: Implications for Red Galaxy Formation

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Extended Red Emission and the evolution of carbonaceous nanograins in NGC 7023

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