HELP project - a dreamed-of multiwavelength dataset for SED fitting: the influence of used models for the main physical properties of galaxies
Katarzyna Malek, Veronique Buat, Denis Burgarella, Yannick Roehlly, Raphael Shirley, HELP team
TTitle of your IAU SymposiumProceedings IAU Symposium No. 341, 2018A.C. Editor, B.D. Editor & C.E. Editor, eds. c (cid:13) HELP pro ject - a dreamed-ofmultiwavelength dataset for SED fitting: theinfluence of used models for the mainphysical properties of galaxies.
Katarzyna Ma(cid:32)lek , , Veronique Buat , Denis Burgarella , YannickRoehlly , , Raphael Shirley and the HELP team National Centre for Nuclear Research, ul.Pasteura 7, 02-093 Warszawa, Poland,email: [email protected] Aix Marseille Univ. CNRS, CNES, LAM Marseille, France, Univ Lyon, Univ Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de LyonUMR5574, F-69230, Saint-Genis-Laval, France Astronomy Centre, Department of Physics and Astronomy, University of Sussex, Falmer,Brighton BN1 9QH, UK
Abstract.
The Herschel Extragalactic Legacy Project (HELP) focuses to publish an astro-nomical multiwavelength catalogue of millions of objects over 1300 deg of the Herschel SpaceObservatory survey fields. Millions of galaxies with ultraviolet–far infrared photometry makeHELP a perfect sample for testing spectral energy distribution fitting models, and to preparetools for next-generation data. In the frame of HELP collaboration we estimated the main phys-ical properties of all galaxies from the HELP database and we checked a new procedure to selectpeculiar galaxies from large galaxy sample and we investigated the influence of used modulesfor stellar mass estimation. Keywords. galaxies: fundamental parameters, infrared, methods: statistical, catalogs
1. Introduction
The primary objective of the Herschel Extragalactic Legacy Project (HELP project,Oliver et al., in preparation, Vaccari 2018) founded by FP7 European Union is to providehomogeneously calibrated multiwavelength catalogues covering roughly 1300 deg of theextragalactic Herschel Space Observatory surveys (HSO, Pilbratt et al. µ m from HSO, depth maps etc. can be found in Shirley et al., 2019 MNRAS (underreview). The catalogues supported by spectroscopic (if possible) or photometric redshift(Duncan et al. a r X i v : . [ a s t r o - ph . GA ] A p r Katarzyna Ma(cid:32)lek & the HELP team
Table 1.
Overview of 23 fields used for HELP project.
HELP field name number of objects area [deg ] AKARI-NEP 531 746 9.2AKARI-SEP 844 172 8.7Bootes 3 367 490 11CDFS-SWIRE 2 171 051 13COSMOS 2 599 374 5.1EGS 1 412 613 3.6ELAIS-N1 4 026 292 14ELAIS-N2 1 783 240 9.2ELAIS-S1 1 655 564 9.0GAMA-09 12 937 982 62GAMA-12 12 369 415 63GAMA-15 14 232 880 62HDF-N 130 679 0.67Herschel-Stripe-82 50 196 455 363Lockman-SWIRE 4 366 298 22HATLAS-NGP 6 759 591 178SA13 9 799 0.27HATLAS-SGP 29 790 690 295SPIRE-NEP 2 674 0.13SSDF 12 661 903 111xFLS 977 148 7.4XMM-13hr 38 629 0.76XMM-LSS 8 704 751 22Total: 171 570 436 1270
2. Data and short overview of the method
The European Large Area ISO Survey North 1 (ELAIS N1, 13.51 deg area centredat 16 h m s +54 o (cid:48) (cid:48)(cid:48) , Oliver et al. 2000) was a pilot field for HELP. The HELPhomogenized catalogue of ELAIS N1 includes 50 135 galaxies with good ultraviolet (UV)–far infrared (IR) measurements (quality criterion requires at least two optical – near IRmeasurements and at least two two of five Herschel measurements with signal to noiseratio (cid:61) et al. (2018).All adopted parameters used for modules are presented in Table. 2. More detaileddiscussion of used parameters and description of addition quality tests for SED fittingprocedure for ELAIS N1 field can be found in Ma(cid:32)lek et al. (2018). An exemplary fit ofSED, showing typical photometric coverage of the spectra is shown in Fig. 1.
3. Impact of the dust attenuation law on the stellar mass
Based on the statistically significant sample of ∼
50 000 galaxies we check the influenceof different dust attenuation recipes on the main physical parameters calculated for allHELP galaxies; stellar mass, star formation rate and dust luminosity. We perform theSED fitting of ELAIS N1 galaxies by assuming three different dust attenuation lawsseparately: Charlot & Fall (2000), widely used in the literature Calzetti et al. (2000),and Lo Faro et al. (2017) – dust attenuation recipe created in the framework of theHELP project for Ultra Luminous Infrared Galaxies at redshift >
2. This test allows us
ELP project - a dreamed-of multiwavelength dataset for SED fitting Table 2.
Main modules and input parameters used in CIGALE for the analysis of the high-zsample. The first column lists the CIGALE model, the second provides a brief description of themain parameters, and the third one shows the range of the selected values.
CIGALE module main parameter description
SFH delayed + additional burst τ of the main stellar population model [Myr] 3 000 τ of the late starburst population model [Myr] 10 000mass fraction of the late burst population 0.001–0.300SSP: Bruzual & Charlot (2003) initial mass function Chabrier (2003)dust attenuation: Charlot & Fall (2000) A V in the BCs 0.3–3.8power law slopes (BC and ISM) -0.7dust emission Draine & Li (2007) minimum radiation field (U min ) 5.0, 10.0, 25.0mass fraction of PAH 1.12, 2.5, 3.19power law slope dU/dM ( U α ) 2.0, 2.8AGN emission: Fritz et al. (2006) fractional contribution of AGN 0.0, 0.15, 0.25, 0.8 Figure 1.
An example of SED fitting result. Open squares represent observed fluxes, whilefilled circles correspond to the model fluxes. The final model is plotted as a solid black line. Therelative residual fluxes are plotted at the bottom of the spectra. to analyze the impact of the assumed law on estimated physical parameters. We findthat the attenuation law has an important impact on the stellar mass estimation (onaverage leading to disparities of a factor of 2), and we derived the relation betweenstellar mass estimates obtained by those three different attenuation laws. Found recipes(published in Ma(cid:32)lel et al. et al. (2000), and Lo Faro et al. (2017),however the attenuation obtained in near infrared band is meaningly different. Similarresult, showing that Calzetti recipe leads to steeper slopes, not consistent with radiationtransfer models results, was found by Buat et al. (2018) based on the infrared completesample of galaxies in the COSMOS 3D-HST CANDELS field at 0.6 < z < et al. (2013)based on the semi-analytic galaxy formation model GALFORM (Cole et al. Figure 2.
Relation between attenuation in near infrared band and attenuation in ultavioletband for all three laws used in the analysis. Open black squares represent Calzetti et al. (2000)recipe, blue dots – Charlot & Fall (2000) law, and orange stars correspond to the Lo Faro et al. (2017) law.
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