SPLASH-SXDF Multi-wavelength Photometric Catalog

Mehta, Vihang; Scarlata, Claudia; Capak, P.; Davidzon, I.; Faisst, Andreas L.; Hsieh, B. C.; Ilbert, O.; Jarvis, Matt J.; Laigle, C.; Phillips, John; Silverman, John D.; Strauss, Michael A.; Tanaka, Masayuki; Bowler, R. A. A.; Coupon, J.; Foucaud, S.; Hemmati, Shoubaneh; Masters, D. C.; McCracken, H. J.; Mobasher, Bahram; Ouchi, Masami; Shibuya, Tetsuo; Wang, Wei-Hao

doi:10.3847/1538-4365/aab60c

Cited by 56 publications

(70 citation statements)

References 87 publications

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“…); Spitzer/IRAC 3.6 µm (ch1) and 4.5 µm (ch2) images from the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH) project (SPLASH; PI: P. Capak et al in prep. ;Mehta et al 2018). All images are publicly available except the SPLASH data.…”

Section: Sxds Fieldmentioning

confidence: 99%

The dominant origin of diffuse Lyα halos around Lyα emitters explored by spectral energy distribution fitting and clustering analysis

Kusakabe

Shimasaku

Momose

et al. 2019

Publications of the Astronomical Society of Japan

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The physical origin of diffuse Lyα halos (LAHs) around star-forming galaxies is still a matter of debate. We present the dependence of LAH luminosity (L(Lyα) H ) on the stellar mass (M ⋆ ), SF R, color excess (E(B − V ) ⋆ ), and dark matter halo mass (M h ) of the parent galaxy for ∼ 900 Lyα emitters (LAEs) at z ∼ 2 divided into ten subsamples. We calculate L(Lyα) H using the stacked observational relation between L(Lyα) H and central Lyα luminosity of Momose et al. (2016, MNRAS, 457, 2318, which we find agrees with the average trend of VLT/MUSEdetected individual LAEs. We find that our LAEs have relatively high L(Lyα) H despite low M ⋆ and M h , and that L(Lyα) H remains almost unchanged with M ⋆ and perhaps with M h . These results are incompatible with the cold stream (cooling radiation) scenario and the satellitegalaxy star-formation scenario, because the former predicts fainter L(Lyα) H and both predict steeper L(Lyα) H vs. M ⋆ slopes. We argue that LAHs are mainly caused by Lyα photons escaping from the main body and then scattered in the circum-galactic medium. This argument is supported by LAH observations of Hα emitters (HAEs). When LAHs are taken into account, the Lyα escape fractions of our LAEs are about ten times higher than those of HAEs with similar M ⋆ or E(B − V ) ⋆ , which may partly arise from lower HI gas masses implied from lower M h at fixed M ⋆ , or from another Lyα source in the central part.

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Section: Sxds Fieldmentioning

confidence: 99%

The dominant origin of diffuse Lyα halos around Lyα emitters explored by spectral energy distribution fitting and clustering analysis

Kusakabe

Shimasaku

Momose

et al. 2019

Publications of the Astronomical Society of Japan

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“…For COSMOS we are using the deep near-IR photometry from UltraVISTA (McCracken et al 2012), taken from the COSMOS2015 catalog (Laigle et al 2016). The near-IR photometry for the SXDS field is taken from the VISTA Deep Extragalactic Observations (VIDEO) survey (Jarvis et al 2013) as provided in the recent SPLASH-SXDF catalog (Mehta et al 2018). For both surveys, we use VISTA J or H magnitudes measured within a 3 ′′ aperture.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…For COSMOS, we utilize the multi-wavelength catalog COSMOS2015 (Laigle et al 2016), where we include homogenized photometry in u * , B, V , g, r, i, z+ from the Canada-France-Hawaii Telescope (CFHT) and Subaru Suprime-Cam, in Y JHK s from VIR-CAM/VISTA (UltraVISTA DR2) and in 3.6µm, 4.5µm, 5.8µm, and 8.0µm from Spitzer-IRAC (S-COSMOS and SPLASH). For SXDS we use the homogenized multiwavelength catalog by Mehta et al (2018). We include data only from the CFHT u-band program MUSUBI, Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP; grizY ), the VISTA Deep Extragalactic Observations (VIDEO) survey (Y JHK s ) and Spitzer-IRAC.…”

Section: Spectral Energy Distribution and Reddeningmentioning

confidence: 99%

See 1 more Smart Citation

An FMOS Survey of Moderate-luminosity, Broad-line AGNs in COSMOS, SXDS, and E-CDF-S

Schulze

Silverman

Kashino

et al. 2018

ApJS

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We present near-IR spectroscopy in J-and H-band for a large sample of 243 X-ray selected moderate-luminosity type-1 AGN in the COSMOS, SXDS and E-CDF-S survey fields using the multiobject spectrograph Subaru/FMOS. Our sample covers the redshift range 0.5 z 3.0 and an X-ray luminosity range of 10 43 L [2−10keV] 10 45 erg s −1 . We provide emission-line properties and derived virial black hole mass estimates, bolometric luminosities and Eddington ratios, based on Hα (211), Hβ (63) and Mg II (4). We compare line widths, luminosities and black hole mass estimates from Hα and Hβ and augment these with commensurate measurements of Mg II and C IV detected in optical spectra. We demonstrate the robustness of using Hα, Hβ and Mg II as reliable black hole mass estimators for high-z moderate-luminosity AGN, while the use of C IV is prone to large uncertainties ( 0.4 dex). We extend a recently proposed correction based on the C IV blueshift to lower luminosities and black hole masses. While our sample shows an improvement in their C IV black hole mass estimates, the deficit of high blueshift sources reduces its overall importance for moderate-luminosity AGN, compared to the most luminous quasars. In addition, we revisit luminosity correlations between L bol , L [2−10keV] , L [OIII] , L 5100 and L Hα and find them to be consistent with a simple empirical model, based on a small number of well-established scaling relations. We finally highlight our highest redshift AGN, CID 781, at z = 4.6 which shows the lowest black hole mass (∼ 10 8 M ⊙ ) among current near-IR samples at this redshift, and is in a state of fast growth.

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“…We collected multi-band photometry in the SPLASH survey data release Mehta et al (2018). We considered optical aperture magnitudes (3 ) from CFHT u filter and from the Hyper Suprime-Cam (HSC) UltraDeep layer in the griz filters; the near-infrared regime is fully covered by the VISTA Deep Extragalactic Observations (VIDEO) Survey Y JHK s aperture magnitudes (3 ), and the mid-infrared takes advantage of the IRAC coverage (ch1, ch2, ch3, ch4) from SPLASH.…”

Section: Sxdfmentioning

confidence: 99%

Euclidpreparation

Guglielmo¹,

Saglia²,

Castander³

et al. 2020

A&A

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The Complete Calibration of the Colour–Redshift Relation survey (C3R2) is a spectroscopic effort involving ESO and Keck facilities designed specifically to empirically calibrate the galaxy colour–redshift relation – P(z|C) to the Euclid depth (iAB = 24.5) and is intimately linked to the success of upcoming Stage IV dark energy missions based on weak lensing cosmology. The aim is to build a spectroscopic calibration sample that is as representative as possible of the galaxies of the Euclid weak lensing sample. In order to minimise the number of spectroscopic observations necessary to fill the gaps in current knowledge of the P(z|C), self-organising map (SOM) representations of the galaxy colour space have been constructed. Here we present the first results of an ESO@VLT Large Programme approved in the context of C3R2, which makes use of the two VLT optical and near-infrared multi-object spectrographs, FORS2 and KMOS. This data release paper focuses on high-quality spectroscopic redshifts of high-redshift galaxies observed with the KMOS spectrograph in the near-infrared H- and K-bands. A total of 424 highly-reliable redshifts are measured in the 1.3 ≤ z ≤ 2.5 range, with total success rates of 60.7% in the H-band and 32.8% in the K-band. The newly determined redshifts fill 55% of high (mainly regions with no spectroscopic measurements) and 35% of lower (regions with low-resolution/low-quality spectroscopic measurements) priority empty SOM grid cells. We measured Hα fluxes in a 1.″2 radius aperture from the spectra of the spectroscopically confirmed galaxies and converted them into star formation rates. In addition, we performed an SED fitting analysis on the same sample in order to derive stellar masses, E(B − V), total magnitudes, and SFRs. We combine the results obtained from the spectra with those derived via SED fitting, and we show that the spectroscopic failures come from either weakly star-forming galaxies (at z < 1.7, i.e. in the H-band) or low S/N spectra (in the K-band) of z > 2 galaxies.

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SPLASH-SXDF Multi-wavelength Photometric Catalog

Cited by 56 publications

References 87 publications

The dominant origin of diffuse Lyα halos around Lyα emitters explored by spectral energy distribution fitting and clustering analysis

The dominant origin of diffuse Lyα halos around Lyα emitters explored by spectral energy distribution fitting and clustering analysis

An FMOS Survey of Moderate-luminosity, Broad-line AGNs in COSMOS, SXDS, and E-CDF-S

Euclidpreparation

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