The VVDS-SWIRE-GALEX-CFHTLS surveys: Physical properties of galaxies at z below 1.2 from photometric data

C. J. Walcher, F. Lamareille, D. Vergani, S. Arnouts, V. Buat, S. Charlot, L. Tresse, O. Le Fèvre, M. Bolzonella, J. Brinchmann, L. Pozzetti, G. Zamorani, D. Bottini, B. Garilli, V. Le Brun, D. Maccagni, B. Milliard, R. Scaramella, M. Scodeggio, G. VettolaniA. Zanichelli, C. Adami, S. Bardelli, A. Cappi, P. Ciliegi, T. Contini, P. Franzetti, S. Foucaud, I. Gavignaud, L. Guzzo, O. Ilbert, A. Iovino, H. J. McCracken, B. Marano, C. Marinoni, A. Mazure, B. Meneux, R. Merighi, S. Paltani, R. Pellò, A. Pollo, M. Radovich, E. Zucca, C. Lonsdale, C. Martin

Resultado de la investigación: Article

54 Citas (Scopus)

Resumen

Measuring the build-up of stellar mass is one of the main objectives of studies of galaxy evolution. Traditionally, the mass in stars and the star formation rates have been measured by different indicators, such as photometric colours, emission lines, and the UV and IR emission. We intend to show that it is possible to derive the physical parameters of galaxies from their broad-band spectral energy distribution out to a redshift of 1.2. This method has the potential to yield the physical parameters of all galaxies in a single field in a homogeneous way, thus overcoming problems with the sample size that particularly plague methods relying on spectroscopy. We use an extensive dataset, assembled in the context of the VVDS survey, which reaches from the UV to the IR and covers a sample of 84 073 galaxies over an area of 0.89 deg 2. We also use a library of 100 000 model galaxies with a wide variety of star formation histories (in particular including late bursts of star formation). We find that we can determine the physical parameters stellar mass, age, and star formation rate with good confidence. We validate the star formation rate determination in particular by comparing it to a sample of spectroscopically observed galaxies with an emission-line measurement. While the attenuation in the galaxies shows more scatter, the mean over the sample is unbiased. Metallicity, however, cannot be measured from rest-frame optical photometry alone. As a first application we use our sample to build the number density function of galaxies as a function of stellar mass, specific star formation rate, and redshift. We are then able to study whether the stellar mass function at a later time can be predicted from the stellar mass function and star formation rate distribution at an earlier time. We find that, between redshifts of 1.02 and 0.47, the predicted growth in stellar mass from star formation agrees with the observed one. However, the predicted stellar mass density for massive galaxies is lower than observed, while the mass density of intermediate mass galaxies is overpredicted. This apparent discrepancy can be explained by major and minor mergers. Indeed, when comparing with a direct measurement of the major merger rate from the VVDS survey, we find that major mergers can account for about half of the mass build-up at the massive end. Minor mergers are very likely to contribute the missing fraction.

Idioma originalEnglish
Páginas (desde-hasta)713-730
Número de páginas18
PublicaciónAstronomy and Astrophysics
Volumen491
N.º3
DOI
EstadoPublished - 1 dic 2008

Huella dactilar

physical property
physical properties
stellar mass
galaxies
star formation rate
merger
star formation
spectral energy distribution
metallicity
photometry
confidence
bursts
rate
attenuation
histories
broadband
spectroscopy
color
stars
history

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Walcher, C. J., Lamareille, F., Vergani, D., Arnouts, S., Buat, V., Charlot, S., ... Martin, C. (2008). The VVDS-SWIRE-GALEX-CFHTLS surveys: Physical properties of galaxies at z below 1.2 from photometric data. Astronomy and Astrophysics, 491(3), 713-730. https://doi.org/10.1051/0004-6361:200810704
Walcher, C. J. ; Lamareille, F. ; Vergani, D. ; Arnouts, S. ; Buat, V. ; Charlot, S. ; Tresse, L. ; Le Fèvre, O. ; Bolzonella, M. ; Brinchmann, J. ; Pozzetti, L. ; Zamorani, G. ; Bottini, D. ; Garilli, B. ; Le Brun, V. ; Maccagni, D. ; Milliard, B. ; Scaramella, R. ; Scodeggio, M. ; Vettolani, G. ; Zanichelli, A. ; Adami, C. ; Bardelli, S. ; Cappi, A. ; Ciliegi, P. ; Contini, T. ; Franzetti, P. ; Foucaud, S. ; Gavignaud, I. ; Guzzo, L. ; Ilbert, O. ; Iovino, A. ; McCracken, H. J. ; Marano, B. ; Marinoni, C. ; Mazure, A. ; Meneux, B. ; Merighi, R. ; Paltani, S. ; Pellò, R. ; Pollo, A. ; Radovich, M. ; Zucca, E. ; Lonsdale, C. ; Martin, C. / The VVDS-SWIRE-GALEX-CFHTLS surveys : Physical properties of galaxies at z below 1.2 from photometric data. En: Astronomy and Astrophysics. 2008 ; Vol. 491, N.º 3. pp. 713-730.
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abstract = "Measuring the build-up of stellar mass is one of the main objectives of studies of galaxy evolution. Traditionally, the mass in stars and the star formation rates have been measured by different indicators, such as photometric colours, emission lines, and the UV and IR emission. We intend to show that it is possible to derive the physical parameters of galaxies from their broad-band spectral energy distribution out to a redshift of 1.2. This method has the potential to yield the physical parameters of all galaxies in a single field in a homogeneous way, thus overcoming problems with the sample size that particularly plague methods relying on spectroscopy. We use an extensive dataset, assembled in the context of the VVDS survey, which reaches from the UV to the IR and covers a sample of 84 073 galaxies over an area of 0.89 deg 2. We also use a library of 100 000 model galaxies with a wide variety of star formation histories (in particular including late bursts of star formation). We find that we can determine the physical parameters stellar mass, age, and star formation rate with good confidence. We validate the star formation rate determination in particular by comparing it to a sample of spectroscopically observed galaxies with an emission-line measurement. While the attenuation in the galaxies shows more scatter, the mean over the sample is unbiased. Metallicity, however, cannot be measured from rest-frame optical photometry alone. As a first application we use our sample to build the number density function of galaxies as a function of stellar mass, specific star formation rate, and redshift. We are then able to study whether the stellar mass function at a later time can be predicted from the stellar mass function and star formation rate distribution at an earlier time. We find that, between redshifts of 1.02 and 0.47, the predicted growth in stellar mass from star formation agrees with the observed one. However, the predicted stellar mass density for massive galaxies is lower than observed, while the mass density of intermediate mass galaxies is overpredicted. This apparent discrepancy can be explained by major and minor mergers. Indeed, when comparing with a direct measurement of the major merger rate from the VVDS survey, we find that major mergers can account for about half of the mass build-up at the massive end. Minor mergers are very likely to contribute the missing fraction.",
keywords = "Galaxies: evolution, Galaxies: general, Galaxies: photometry, Surveys",
author = "Walcher, {C. J.} and F. Lamareille and D. Vergani and S. Arnouts and V. Buat and S. Charlot and L. Tresse and {Le F{\`e}vre}, O. and M. Bolzonella and J. Brinchmann and L. Pozzetti and G. Zamorani and D. Bottini and B. Garilli and {Le Brun}, V. and D. Maccagni and B. Milliard and R. Scaramella and M. Scodeggio and G. Vettolani and A. Zanichelli and C. Adami and S. Bardelli and A. Cappi and P. Ciliegi and T. Contini and P. Franzetti and S. Foucaud and I. Gavignaud and L. Guzzo and O. Ilbert and A. Iovino and McCracken, {H. J.} and B. Marano and C. Marinoni and A. Mazure and B. Meneux and R. Merighi and S. Paltani and R. Pell{\`o} and A. Pollo and M. Radovich and E. Zucca and C. Lonsdale and C. Martin",
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Walcher, CJ, Lamareille, F, Vergani, D, Arnouts, S, Buat, V, Charlot, S, Tresse, L, Le Fèvre, O, Bolzonella, M, Brinchmann, J, Pozzetti, L, Zamorani, G, Bottini, D, Garilli, B, Le Brun, V, Maccagni, D, Milliard, B, Scaramella, R, Scodeggio, M, Vettolani, G, Zanichelli, A, Adami, C, Bardelli, S, Cappi, A, Ciliegi, P, Contini, T, Franzetti, P, Foucaud, S, Gavignaud, I, Guzzo, L, Ilbert, O, Iovino, A, McCracken, HJ, Marano, B, Marinoni, C, Mazure, A, Meneux, B, Merighi, R, Paltani, S, Pellò, R, Pollo, A, Radovich, M, Zucca, E, Lonsdale, C & Martin, C 2008, 'The VVDS-SWIRE-GALEX-CFHTLS surveys: Physical properties of galaxies at z below 1.2 from photometric data', Astronomy and Astrophysics, vol. 491, n.º 3, pp. 713-730. https://doi.org/10.1051/0004-6361:200810704

The VVDS-SWIRE-GALEX-CFHTLS surveys : Physical properties of galaxies at z below 1.2 from photometric data. / Walcher, C. J.; Lamareille, F.; Vergani, D.; Arnouts, S.; Buat, V.; Charlot, S.; Tresse, L.; Le Fèvre, O.; Bolzonella, M.; Brinchmann, J.; Pozzetti, L.; Zamorani, G.; Bottini, D.; Garilli, B.; Le Brun, V.; Maccagni, D.; Milliard, B.; Scaramella, R.; Scodeggio, M.; Vettolani, G.; Zanichelli, A.; Adami, C.; Bardelli, S.; Cappi, A.; Ciliegi, P.; Contini, T.; Franzetti, P.; Foucaud, S.; Gavignaud, I.; Guzzo, L.; Ilbert, O.; Iovino, A.; McCracken, H. J.; Marano, B.; Marinoni, C.; Mazure, A.; Meneux, B.; Merighi, R.; Paltani, S.; Pellò, R.; Pollo, A.; Radovich, M.; Zucca, E.; Lonsdale, C.; Martin, C.

En: Astronomy and Astrophysics, Vol. 491, N.º 3, 01.12.2008, p. 713-730.

Resultado de la investigación: Article

TY - JOUR

T1 - The VVDS-SWIRE-GALEX-CFHTLS surveys

T2 - Physical properties of galaxies at z below 1.2 from photometric data

AU - Walcher, C. J.

AU - Lamareille, F.

AU - Vergani, D.

AU - Arnouts, S.

AU - Buat, V.

AU - Charlot, S.

AU - Tresse, L.

AU - Le Fèvre, O.

AU - Bolzonella, M.

AU - Brinchmann, J.

AU - Pozzetti, L.

AU - Zamorani, G.

AU - Bottini, D.

AU - Garilli, B.

AU - Le Brun, V.

AU - Maccagni, D.

AU - Milliard, B.

AU - Scaramella, R.

AU - Scodeggio, M.

AU - Vettolani, G.

AU - Zanichelli, A.

AU - Adami, C.

AU - Bardelli, S.

AU - Cappi, A.

AU - Ciliegi, P.

AU - Contini, T.

AU - Franzetti, P.

AU - Foucaud, S.

AU - Gavignaud, I.

AU - Guzzo, L.

AU - Ilbert, O.

AU - Iovino, A.

AU - McCracken, H. J.

AU - Marano, B.

AU - Marinoni, C.

AU - Mazure, A.

AU - Meneux, B.

AU - Merighi, R.

AU - Paltani, S.

AU - Pellò, R.

AU - Pollo, A.

AU - Radovich, M.

AU - Zucca, E.

AU - Lonsdale, C.

AU - Martin, C.

PY - 2008/12/1

Y1 - 2008/12/1

N2 - Measuring the build-up of stellar mass is one of the main objectives of studies of galaxy evolution. Traditionally, the mass in stars and the star formation rates have been measured by different indicators, such as photometric colours, emission lines, and the UV and IR emission. We intend to show that it is possible to derive the physical parameters of galaxies from their broad-band spectral energy distribution out to a redshift of 1.2. This method has the potential to yield the physical parameters of all galaxies in a single field in a homogeneous way, thus overcoming problems with the sample size that particularly plague methods relying on spectroscopy. We use an extensive dataset, assembled in the context of the VVDS survey, which reaches from the UV to the IR and covers a sample of 84 073 galaxies over an area of 0.89 deg 2. We also use a library of 100 000 model galaxies with a wide variety of star formation histories (in particular including late bursts of star formation). We find that we can determine the physical parameters stellar mass, age, and star formation rate with good confidence. We validate the star formation rate determination in particular by comparing it to a sample of spectroscopically observed galaxies with an emission-line measurement. While the attenuation in the galaxies shows more scatter, the mean over the sample is unbiased. Metallicity, however, cannot be measured from rest-frame optical photometry alone. As a first application we use our sample to build the number density function of galaxies as a function of stellar mass, specific star formation rate, and redshift. We are then able to study whether the stellar mass function at a later time can be predicted from the stellar mass function and star formation rate distribution at an earlier time. We find that, between redshifts of 1.02 and 0.47, the predicted growth in stellar mass from star formation agrees with the observed one. However, the predicted stellar mass density for massive galaxies is lower than observed, while the mass density of intermediate mass galaxies is overpredicted. This apparent discrepancy can be explained by major and minor mergers. Indeed, when comparing with a direct measurement of the major merger rate from the VVDS survey, we find that major mergers can account for about half of the mass build-up at the massive end. Minor mergers are very likely to contribute the missing fraction.

AB - Measuring the build-up of stellar mass is one of the main objectives of studies of galaxy evolution. Traditionally, the mass in stars and the star formation rates have been measured by different indicators, such as photometric colours, emission lines, and the UV and IR emission. We intend to show that it is possible to derive the physical parameters of galaxies from their broad-band spectral energy distribution out to a redshift of 1.2. This method has the potential to yield the physical parameters of all galaxies in a single field in a homogeneous way, thus overcoming problems with the sample size that particularly plague methods relying on spectroscopy. We use an extensive dataset, assembled in the context of the VVDS survey, which reaches from the UV to the IR and covers a sample of 84 073 galaxies over an area of 0.89 deg 2. We also use a library of 100 000 model galaxies with a wide variety of star formation histories (in particular including late bursts of star formation). We find that we can determine the physical parameters stellar mass, age, and star formation rate with good confidence. We validate the star formation rate determination in particular by comparing it to a sample of spectroscopically observed galaxies with an emission-line measurement. While the attenuation in the galaxies shows more scatter, the mean over the sample is unbiased. Metallicity, however, cannot be measured from rest-frame optical photometry alone. As a first application we use our sample to build the number density function of galaxies as a function of stellar mass, specific star formation rate, and redshift. We are then able to study whether the stellar mass function at a later time can be predicted from the stellar mass function and star formation rate distribution at an earlier time. We find that, between redshifts of 1.02 and 0.47, the predicted growth in stellar mass from star formation agrees with the observed one. However, the predicted stellar mass density for massive galaxies is lower than observed, while the mass density of intermediate mass galaxies is overpredicted. This apparent discrepancy can be explained by major and minor mergers. Indeed, when comparing with a direct measurement of the major merger rate from the VVDS survey, we find that major mergers can account for about half of the mass build-up at the massive end. Minor mergers are very likely to contribute the missing fraction.

KW - Galaxies: evolution

KW - Galaxies: general

KW - Galaxies: photometry

KW - Surveys

UR - http://www.scopus.com/inward/record.url?scp=57049098264&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:200810704

DO - 10.1051/0004-6361:200810704

M3 - Article

AN - SCOPUS:57049098264

VL - 491

SP - 713

EP - 730

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

IS - 3

ER -