Photometric redshifts from evolutionary synthesis with PÉGASE: The code Z-PEG and the z=0 age constraint

By D. L. Borgne, Brigitte Rocca-Volmerange Institut d'astrophysique de Paris, I. D. Spatiale. 2002

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Photometric redshifts are estimated on the basis of template scenarios with the help of the code Z-PEG, an extension of the galaxy evolution model P EGASE.2 and available on the P EGASE web site. The spectral energy distribution (SED) templates are computed for nine spectral types including starburst, irregular, spiral and elliptical. Dust, extinction and metal eects are coherently taken into account, depending on evolution scenarios. The sensitivity of results to adding near-infrared colors and IGM absorption is analyzed. A comparison with results of other models without evolution measures the evolution factor which systematically increases the estimated photometric redshift values byz 0:2 for z> 1:5. Moreover we systematically check that the evolution scenarios match observational standard templates of nearby galaxies, implying an age constraint of the stellar population at z = 0 for each type. The respect of this constraint makes it possible to signicantly improve the accuracy of photometric redshifts by decreasing the well-known degeneracy problem. The method is applied to the HDF-N sample (see in Fern andez-Soto et al. 1999). From ts on SED templates by a 2 -minimization procedure, not only is the photometric redshift derived but also the corresponding spectral type and the formation redshift zfor when stars rst formed. Early epochs of galaxy formationzfor > 5 are found from this new method and results are compared to faint galaxy count interpretations. The new tool is available at: http://www.iap.fr/pegase

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c2671447a7eb6adb8f03b67b570ddbe56c813fea

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Citations in the corpus

Rates and Properties of Type Ia Supernovae as a Function of Mass and Star Formation in Their Host Galaxies (2006, methodology): “This technique is similar to that employed by photometric redshift codes (e.g. Gwyn & Hartwick 1996; Bolzonella et al. 2000; Le Borgne & Rocca-Volmerange 2002).”
The reversal of the star formation-density relation in the distant universe (2007, methodology): “…of the GOODS spectroscopic sample inside the redshift range of interesth re (0.8≤ z ≤1.2), we used the large number of passbands available in the GOODS fields (UBVRIzJHK,3.6µm,4.5µm) to derive photometric redshifts with an accuracy of∆z/(1+z)=0.05– 1 using Z-PEG (Le Borgne & Rocca-Volmerange 2002).”
The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample (2017, methodology): “The measured magnitudes are analyzed with the photometric redshift code Z-PEG (Le Borgne & Rocca-Volmerange 2002), which is based on the PEGASE.2 spectral synthesis code (Fioc & Rocca-Volmerange 1999) and follows da Cunha et al. (2012) to calculate the stellar masses of host galaxies.”
A CONTINUUM OF H- TO He-RICH TIDAL DISRUPTION CANDIDATES WITH A PREFERENCE FOR E+A GALAXIES (2014, methodology): “Host Galaxies We obtain ugriz magnitudes of all host galaxies from SDSS DR10 and analyze them using z-peg (Le Borgne & Rocca-Volmerange 2002), which is based on the spectral synthesis code PEGASE.2 (Fioc & Rocca-Volmerange 1997). z-peg fits the observed galaxy magnitudes with SED templates (of SB,…”
A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, methodology): “Masses are determined using the method describe in Le Borgne & Rocca-Volmerange (2002) and as used in E07 and E11.”
Evolutionary synthesis of galaxies at high spectral resolution with the code PEGASE-HR. Metallicity and age tracers (2004, result): “Figure 14 shows the predictions of the main Lick indices with our three scenarios (spiral, elliptical, and instantaneous burst, as defined in Le Borgne & Rocca-Volmerange 2002) compared to the same indices measured on local elliptical galaxies (Trager et al. 2000).”
The Infrared Luminosity Function of Galaxies at Redshifts z = 1 and z ~ 2 in the GOODS Fields (2007, methodology): “Thus, to test these possible spurious redshifts, we double-checked the fitting of all the galaxies with HYPERZ redshift 1.5 zphot 1.7 using the PÉGASE library (Le Borgne & Rocca-Volmerange 2002).”
The dependence of Type Ia Supernovae luminosities on their host galaxies (2010, methodology): “The method to estimate physical parameters of the SN Ia host galaxies is similar to that in S06 which used the photometric redshift code ZPEG (Le Borgne & Rocca-Volmerange 2002) based upon the PÉGASE.2 spectral synthesis code (e.g., Fioc & Rocca-Volmerange 1997).”
The evolution of the luminosity functions in the FORS Deep Field from low to high redshift: I. The blue bands (2004, methodology): “Several methods have been described in the literature to derive photometric redshifts (Baum, 1962; Koo, 1985; Brunner et al., 1999; Fernández-Soto et al., 1999; Beńıtez, 2000; Le Borgne & Rocca-Volmerange, 2002; Firth et al., 2003).”
SUPERNOVA CONSTRAINTS AND SYSTEMATIC UNCERTAINTIES FROM THE FIRST THREE YEARS OF THE SUPERNOVA LEGACY SURVEY (2011, methodology): “…for including host-galaxy information in the cosmological fits to correct for the dependence of SN residual from the Hubble relationship; see that paper for the details of how we measure host-galaxy parameters using broad band photometry and the Z-PEG package (Le Borgne & Rocca-Volmerange 2002).”
High luminosity, slow ejecta and persistent carbon lines: SN 2009dc challenges thermonuclear explosion scenarios (2010, methodology): “We then used ZPEG (Le Borgne & Rocca-Volmerange 2002) to match our photometry to galaxy evolutionary scenarios.”
The Progenitors of Type Ia Supernovae (2008, methodology): “Models with exponentially decreasing SFR(t) match the locus of the SFR ∝ t−p models, as do models constructed using the PEGASE.2 evolutionary infall scenario (Le Borgne & Rocca-Volmerange 2002).”
The GOODS-MUSIC sample: a multicolour catalog of near-IR selected galaxies in the GOODS-South field , (2006, methodology): “Another differences in our approach compared to Le Borgne & Rocca-Volmerange (2002) are that we do not apply any constraint on the galaxy ages (apart from those set by the Hubble time at each z) and that we have allowed for a finer time sampling in the galaxy ages by halving the time step with…”
THE EFFECT OF HOST GALAXIES ON TYPE Ia SUPERNOVAE IN THE SDSS-II SUPERNOVA SURVEY (2010, methodology): “In detail, we used the eight star-forming scenarios, as listed in Table 1 of Le Borgne & Rocca-Volmerange (2002), and assume a Kroupa (2001) initial mass function.”
The 0.4 < z < 1.3 star formation history of the Universe as viewed in the far-infrared (2009, methodology): “For the GOODS fields, we complemented the spectroscopic redshifts with photometric redshifts estimated using Z-PEG (Le Borgne & Rocca-Volmerange 2002).”
Photometric redshifts in the SWIRE Survey (2008, background): “…et al 1999, 2002, Benitez 2000, Fontana et al 2000, Bolzonella et al 2000, Thompson et al 2001, Teplitz et al 2001, Lanzetta et al 2002, Le Borgne and Rocca-Volmerange 2002, Firth et al 2002, 2003, Chen and Lanzetta 2003, RowanRobinson 2003, Wolf et al 2004, Rowan-Robinson et al 2004,…”