Candels Multi-Wavelength Catalogs: Source Identification and Photometry in the Candels Cosmos Survey Field

Nayyeri, Hooshang; Hemmati, Shoubaneh; Mobasher, Bahram; Ferguson, Harry; Cooray, Asantha; Barro, Guillermo; Faber, S. M.; Dickinson, Mark; Koekemoer, Anton M.; Peth, Michael; Salvato, M.; Ashby, M. L. N.; Darvish, Behnam; Donley, J. L.; Durbin, Meredith; Finkelstein, Steven L.; Fontana, A.; Grogin, Norman A.; Gruetzbauch, Ruth; Huang, K. H.; Khostovan, Ali Ahmad; Kocevski, Dale D.; Kodra, Dritan; Lee, B.; Newman, Jeffrey A.; Pacifici, Camilla; Pforr, Janine; Stefanon, Mauro; Wiklind, T.; Willner, S. P.; Wuyts, Stijn; Castellano, M.; Conselice, Christopher J.; Dolch, Timothy; Dunlop, James; Galametz, A.; Hathi, N. P.; Lucas, Ray A.; Yan, Haojing

doi:10.3847/1538-4365/228/1/7

Cited by 128 publications

(108 citation statements)

References 178 publications

(352 reference statements)

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“…K) band selection, as done in previous analyses. Deeper HST data available in the overlap with the CANDELS field (Nayyeri et al 2017) have been used to confirm the absence of significant biases in our final sample, cut at [3.6] < 25.…”

Section: Discussionmentioning

confidence: 99%

The COSMOS2015 galaxy stellar mass function

Davidzon

Ilbert

Laigle

et al. 2017

A&A

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423

613

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We measure the stellar mass function (SMF) and stellar mass density of galaxies in the COSMOS field up to z ∼ 6. We select them in the near-IR bands of the COSMOS2015 catalogue, which includes ultra-deep photometry from UltraVISTA-DR2, SPLASH, and Subaru/Hyper SuprimeCam. At z > 2.5 we use new precise photometric redshifts with error σ z = 0.03(1 + z) and an outlier fraction of 12%, estimated by means of the unique spectroscopic sample of COSMOS (∼100 000 spectroscopic measurements in total, more than one thousand having robust z spec > 2.5). The increased exposure time in the DR2, along with our panchromatic detection strategy, allow us to improve the completeness at high z with respect to previous UltraVISTA catalogues (e.g. our sample is >75% complete at 10 10 M and z = 5). We also identify passive galaxies through a robust colour-colour selection, extending their SMF estimate up to z = 4. Our work provides a comprehensive view of galaxy-stellar-mass assembly between z = 0.1 and 6, for the first time using consistent estimates across the entire redshift range. We fit these measurements with a Schechter function, correcting for Eddington bias. We compare the SMF fit with the halo mass function predicted from ΛCDM simulations, finding that at z > 3 both functions decline with a similar slope in the high-mass end. This feature could be explained assuming that mechanisms quenching star formation in massive haloes become less effective at high redshifts; however further work needs to be done to confirm this scenario. Concerning the SMF low-mass end, it shows a progressive steepening as it moves towards higher redshifts, with α decreasing from −1.47 +0.02 −0.02 at z 0.1 to −2.11 +0.30 −0.13 at z 5. This slope depends on the characterisation of the observational uncertainties, which is crucial to properly remove the Eddington bias. We show that there is currently no consensus on the method to quantify such errors: different error models result in different best-fit Schechter parameters.

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Section: Discussionmentioning

confidence: 99%

The COSMOS2015 galaxy stellar mass function

Davidzon

Ilbert

Laigle

et al. 2017

A&A

Self Cite

423

613

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“…Such systematics in the measurement of stellar mass introduces up to ∼ 0.5 dex offset in the number densities for the higher redshift bins. To further complicate the picture, recent works have shown that when the correction for nebular line contamination is applied on a statistical basis, irrespective of the specific SEDs, it can even boost the stellar mass measurements by up to ∼ 0.2 − 0.3 dex (Stefanon et al 2015;Stefanon 2017;Nayyeri et al 2017).…”

Section: Schechter Best-fit To the Lf And Smfmentioning

confidence: 99%

The Rest-frame Optical (900 nm) Galaxy Luminosity Function at z ∼ 4–7: Abundance Matching Points to Limited Evolution in the M_STAR/M_HALO Ratio at z ≥ 4

Stefanon

Bouwens

Labbé

et al. 2017

ApJ

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We present the first determination of the galaxy luminosity function (LF) at z ∼ 4, 5, 6 and 7 in the rest-frame optical at λ rest ∼ 900 nm (z ′ band). The rest-frame optical light traces the content in lowmass evolved stars (∼stellar mass -M * ), minimizing potential measurement biases for M * . Moreover it is less affected by nebular line emission contamination and dust attenuation, is independent of stellar population models, and can be probed up to z ∼ 8 through Spitzer/IRAC. Our analysis leverages the unique full depth Spitzer /IRAC 3.6µm-to-8.0µm data over the CANDELS/GOODS-N, CANDELS/GOODS-S and COSMOS/UltraVISTA fields. We find that at absolute magnitudes M z ′ fainter than −23 mag, M z ′ linearly correlates with M UV,1600 . At brighter M z ′ , M UV,1600 presents a turnover, suggesting that the stellar mass-to-light ratio M * /L UV,1600 could be characterised by a very broad range of values at high stellar masses. Median-stacking analyses recover a M * /L z ′ roughly independent on M z ′ for M z ′ −23 mag, but exponentially increasing at brighter magnitudes. We find that the evolution of the LF marginally prefers a pure luminosity evolution over a pure density evolution, with the characteristic luminosity decreasing by a factor ∼ 5× between z ∼ 4 and z ∼ 7. Direct application of the recovered M * /L z ′ generates stellar mass functions consistent with average measurements from the literature. Measurements of the stellar-to-halo mass ratio at fixed cumulative number density show that it is roughly constant with redshift for M h 10 12 M ⊙ . This is also supported by the fact that the evolution of the LF at 4 z 7 can be accounted for by a rigid displacement in luminosity corresponding to the evolution of the halo mass from abundance matching.

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“…Similar to all the rest of the CANDELS fields (Guo et al 2013;Galametz et al 2013;G. Barro et al 2017, in preparation;Nayyeri et al 2017), object detection was performed on the WFC3/F160W-band image. This mosaic is fully covered by all the adopted data sets, with the exception of the data from the NMBS and the WFC3 F140W mosaic,which cover only about one-thirdand two-thirdsof the F160W field respectively (see Figure 2).…”

Section: Datamentioning

confidence: 99%

“…The CANDELS GOODS-S data, combined withthe medium bands from Subaru (Cardamone et al 2010), were also used in Hsu et al (2014) to compute photometric redshifts of normal galaxies and AGNs. The description of the multi-wavelength catalogs, photometric redshifts, and stellar population parameters for the COSMOS and GOODS-N fields are presented by Nayyeri et al (2017) and G. Barro et al (2017, in preparation), respectively. This paper presents the CANDELS multi-wavelength photometric catalog for the EGS field.…”

Section: Introductionmentioning

confidence: 99%

CANDELS Multi-wavelength Catalogs: Source Identification and Photometry in the CANDELS Extended Groth Strip

Stefanon

Yan

Mobasher

et al. 2017

ApJS

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188

159

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We present a 0.4-8 μm multi-wavelength photometric catalog in the Extended Groth Strip (EGS) field. This catalog is built on the Hubble Space Telescope (HST) WFC3 and ACS data from the Cosmic Assembly Nearinfrared Deep Extragalactic Legacy Survey (CANDELS), and it incorporates the existing HST data from the Allwavelength Extended Groth strip International Survey (AEGIS) and the 3D-HST program. The catalog is based on detections in the F160W band reaching a depth of F160W=26.62 AB (90% completeness, point sources). It includes the photometry for 41,457 objects over an area of »206 arcmin 2 in the following bands: HST/ACS F606W and F814W; HST WFC3 F125W, F140W, and F160W; Canada-France-Hawaii Telescope (CFHT)/ Megacam u * , ¢ g , ¢ r , ¢ i and ¢ z ; CFHT/WIRCAM J, H,and K S ; Mayall/NEWFIRM J1, J2, J3, H1, H2, and K; Spitzer IRAC 3.6, 4.5, 5.8, and 8.0 μm. We are also releasing value-added catalogs that provide robust photometric redshifts and stellar mass measurements. The catalogs are publicly available through the CANDELS repository.

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Candels Multi-Wavelength Catalogs: Source Identification and Photometry in the Candels Cosmos Survey Field

Cited by 128 publications

References 178 publications

The COSMOS2015 galaxy stellar mass function

The COSMOS2015 galaxy stellar mass function

The Rest-frame Optical (900 nm) Galaxy Luminosity Function at z ∼ 4–7: Abundance Matching Points to Limited Evolution in the M_STAR/M_HALO Ratio at z ≥ 4

CANDELS Multi-wavelength Catalogs: Source Identification and Photometry in the CANDELS Extended Groth Strip

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Candels Multi-Wavelength Catalogs: Source Identification and Photometry in the Candels Cosmos Survey Field

Cited by 128 publications

References 178 publications

The COSMOS2015 galaxy stellar mass function

The COSMOS2015 galaxy stellar mass function

The Rest-frame Optical (900 nm) Galaxy Luminosity Function at z ∼ 4–7: Abundance Matching Points to Limited Evolution in the MSTAR/MHALO Ratio at z ≥ 4

CANDELS Multi-wavelength Catalogs: Source Identification and Photometry in the CANDELS Extended Groth Strip

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Product

Resources

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The Rest-frame Optical (900 nm) Galaxy Luminosity Function at z ∼ 4–7: Abundance Matching Points to Limited Evolution in the M_STAR/M_HALO Ratio at z ≥ 4