The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Scodeggio, M.; Guzzo, L.; Garilli, B.; Granett, B. R.; Bolzonella, M.; Torre, S. de la; Abbas, U.; Adami, C.; Arnouts, S.; Bottini, D.; Cappi, A.; Coupon, J.; Cucciati, O.; Davidzon, I.; Franzetti, P.; Fritz, A.; Iovino, A.; Krywult, J.; Brun, V. Le; Fèvre, O. Le; Maccagni, D.; Małek, K.; Marchetti, A.; Marulli, F.; Polletta, M.; Pollo, A.; Tasca, L.; Tojeiro, Rita; Vergani, D.; Zanichelli, A.; Bel, J.; Branchini, E.; Lucia, G. De; Ilbert, O.; McCracken, H. J.; Moutard, T.; Peacock, J. A.; Zamorani, G.; Burden, A.; Fumana, M.; Jullo, Eric; Marinoni, C.; Mellier, Y.; Moscardini, L.; Percival, Will J.

doi:10.1051/0004-6361/201630114

Cited by 205 publications

(200 citation statements)

References 27 publications

(36 reference statements)

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“…The vast majority of them (30 out of 33) come from the SDSS (DR15) survey. The remaining optical spectra are from the Galaxy And Mass Assembly (GAMA; Driver et al 2011;Baldry et al 2010) and the VIPERS (Guzzo et al 2014;Scodeggio et al 2018) surveys. In our analysis, we use spectroscopic redshifts for 33 sources.…”

Section: Red Agnsmentioning

confidence: 99%

The XXL Survey

Masoura

Georgantopoulos

Mountrichas

et al. 2020

A&A

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The combination of optical and mid-infrared (MIR) photometry has been extensively used to select red active galactic nuclei (AGNs). Our aim is to explore the obscuration properties of these red AGNs with both X-ray spectroscopy and spectral energy distributions (SEDs). In this study, we re-visit the relation between optical/MIR extinction and X-ray absorption. We use IR selection criteria, specifically the W1 and W2 WISE bands, to identify 4798 AGNs in the XMM − XXL area (∼ 25 deg 2 ). Application of optical/MIR colours (r − W2 > 6) reveals 561 red AGNs (14%). Of these, 47 have available X-ray spectra with at least 50 net (backgroundsubtracted) counts per detector. For these sources, we construct SEDs from the optical to the MIR using the CIGALE code. The SED fitting shows that 44 of these latter 47 sources present clear signs of obscuration based on the AGN emission and the estimated inclination angle. Fitting the SED also reveals ten systems (∼ 20%) which are dominated by the galaxy. In these cases, the red colours are attributed to the host galaxy rather than AGN absorption. Excluding these ten systems from our sample and applying X-ray spectral fitting analysis shows that up to 76% (28/37) of the IR red AGNs present signs of X-ray absorption. Thus, there are nine sources (∼ 20% of the sample) that although optically red, are not substantially X-ray absorbed. Approximately 50% of these sources present broad emission lines in their optical spectra. We suggest that the reason for this apparent discrepancy is that the r-W2 criterion is sensitive to smaller amounts of obscuration relative to the X-ray spectroscopy. In conclusion, it appears that the majority of red AGNs present considerable obscuration levels as shown by their SEDs. Their X-ray absorption is moderate with a mean of N H ∼ 10 22 cm −2 .

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Section: Red Agnsmentioning

confidence: 99%

The XXL Survey

Masoura

Georgantopoulos

Mountrichas

et al. 2020

A&A

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“…Data VIPERS 1 (Guzzo et al 2014;Scodeggio et al 2017) has measured redshifts for ∼10 5 galaxies at redshift 0.5 < z 1.2. The project had two broad scientific goals: i) to reliably measure galaxy clustering and the growth of structure through redshiftspace distortions; ii) to study galaxy properties at an epoch when the Universe was about half its current age, over a volume comparable to that of large existing local (z ∼ 0.1) surveys, like 2dF-GRS and SDSS.…”

Section: Data and Mock Samplesmentioning

confidence: 99%

“…The number of slits in each VIMOS pointing was maximised using the SSPOC algorithm (Bottini et al 2005). The typical radial velocity error on the spectroscopic redshift (z s ) measurement of a galaxy is σ z = 0.00054(1 + z) (see Scodeggio et al 2017, for more details). A discussion of the survey data reduction and database system is presented in Garilli et al (2012).…”

Section: Data and Mock Samplesmentioning

confidence: 99%

“…The data used here correspond to the publicly released PDR-2 catalogue (Scodeggio et al 2017), with the exception of a small sub-set of redshifts (340 galaxies missing in the range 0.6 < z < 1.1), for which the redshift and quality flags were revised closer to the release date. Concerning the analysis presented here, this has no effect.…”

Section: Data and Mock Samplesmentioning

confidence: 99%

“…The quality flag is assigned to each targeted object during the process of validating redshift measurements, according to a scheme that has been adopted by previous VIMOS surveys (VVDS, Le Fèvre et al 2005;and zCOSMOS, Lilly et al 2009). The average confidence level of single redshift measurements for the sample of reliable redshifts is estimated to be 96.1% (Scodeggio et al 2017). In our case, this selection produces a sample of 74 835 galaxies.…”

Section: Data and Mock Samplesmentioning

confidence: 99%

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The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Cucciati

Davidzon

Bolzonella

et al. 2017

A&A

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We use the final data of the VIMOS Public Extragalactic Redshift Survey (VIPERS) to investigate the effect of the environment on the evolution of galaxies between z = 0.5 and z = 0.9. We characterise local environment in terms of the density contrast smoothed over a cylindrical kernel, the scale of which is defined by the distance to the fifth nearest neighbour. This is performed by using a volume-limited sub-sample of galaxies complete up to z = 0.9, but allows us to attach a value of local density to all galaxies in the full VIPERS magnitude-limited sample to i < 22.5. We use this information to estimate how the distribution of galaxy stellar masses depends on environment. More massive galaxies tend to reside in higher-density environments over the full redshift range explored. Defining star-forming and passive galaxies through their (NUV−r) vs. (r − K) colours, we then quantify the fraction of star-forming over passive galaxies, f ap , as a function of environment at fixed stellar mass. f ap is higher in low-density regions for galaxies with masses ranging from log(M/M ) = 10.38 (the lowest value explored) to at least log(M/M ) ∼ 11.3, although with decreasing significance going from lower to higher masses. This is the first time that environmental effects on high-mass galaxies are clearly detected at redshifts as high as z ∼ 0.9. We compared these results to VIPERS-like galaxy mock catalogues based on a widely used galaxy formation model. The model correctly reproduces f ap in low-density environments, but underpredicts it at high densities. The discrepancy is particularly strong for the lowest-mass bins. We find that this discrepancy is driven by an excess of low-mass passive satellite galaxies in the model. In high-density regions, we obtain a better (although not perfect) agreement of the model f ap with observations by studying the accretion history of these model galaxies (that is, the times when they become satellites), by assuming either that a non-negligible fraction of satellites is destroyed, or that their quenching timescale is longer than ∼2 Gyr.

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