The MUSE-Wide Survey: survey description and first data release

Abstract

We present the MUSE-Wide survey, a blind, 3D spectroscopic survey in the CANDELS/GOODS-S and CANDELS/COSMOS regions. The final survey will cover 100 × 1 arcmin 2 MUSE fields. Each MUSE-Wide pointing has a depth of 1 hour and hence targets more extreme and more luminous objects over 10 times the area of the MUSE-Deep fields . The legacy value of MUSE-Wide lies in providing "spectroscopy of everything" without photometric pre-selection. We describe the data reduction, post-processing and PSF characterization of the first 44 CANDELS/GOODS-S MUSE-Wide pointings released with this publication. Using a 3D matched filtering approach we detect 1,602 emission line sources, including 479 Lyman-α (Lyα) emitting galaxies with redshifts 2.9 z 6.3. We cross-match the emission line sources to existing photometric catalogs, finding almost complete agreement in redshifts (photometric and spectroscopic) and stellar masses for our low redshift (z < 1.5) emitters. At high redshift, we only find ∼55% matches to photometric catalogs. We encounter a higher outlier rate and a systematic offset of ∆z 0.2 when comparing our MUSE redshifts with photometric redshifts from the literature. Cross-matching the emission line sources with X-ray catalogs from the Chandra Deep Field South, we find 127 matches, mostly in agreement with the literature redshifts, including 10 objects with no prior spectroscopic identification. Stacking X-ray images centered on our Lyα emitters yields no signal; the Lyα population is not dominated by even low luminosity AGN. Other cross-matches of our emission-line catalog to radio and submm data, yielded far lower numbers of matches, most of which already were covered by the X-ray catalog. A total of 9,205 photometrically selected objects from the CANDELS survey lie in the MUSE-Wide footprint, which we provide optimally extracted 1D spectra of. We are able to determine the spectroscopic redshift of 98% of 772 photometrically selected galaxies brighter than 24th F775W magnitude. All the data in the first data release -datacubes, catalogs, extracted spectra, maps -are available on the website https://musewide.aip.de.

Spatially Resolved Properties of Galaxies from CANDELS+MUSE: Radial Extinction Profile and Insights on Quenching

“…In recent years, spatially-resolved spectroscopy of local galaxies became feasible thanks to the integral field spectroscopy (IFS) surveys, such as SAMI (Croom et al 2012;Scott et al 2018), CALIFA (Sánchez et al 2012), and MaNGA (Bundy et al 2015). For this work, we needed IFS data in a field with available high spatial resolution multi-waveband photometry, so we take advantage of MUSE-Wide Survey (Urrutia et al 2019) which also allowed us to go further than previous studies by examining the resolved properties of galaxies at lower masses and higher redshifts. We focus on studying radial profiles of SFR, sSFR and dust attenuation in a sample of 32 galaxies with high S/N detection of Hα and Hβ at 0.1 < z < 0.42 and average stellar mass of 10 8.71 M .…”

Constraining Lyman-alpha spatial offsets at 3 &lt; z &lt; 5.5 from VANDELS slit spectroscopy

“…Astrometry issues aside, MUSE has a limited FOV (∼ 1 arcmin 2 ), so a statistical measurement of Lyα spatial offsets would require many MUSE pointings. The MUSE-Wide survey (Urrutia et al 2019) is currently in progress to obtain 100 MUSE pointings at 1 hr per pointing. Assuming the astrometric issues mentioned by Wisotzki et al (2016) can be overcome, this may be a promising avenue to constrain Lyα spatial offsets.…”

A Submillimeter Perspective on the GOODS Fields (SUPER GOODS). IV. The Submillimeter Properties of X-Ray Sources in the CDF-S

“…Chandra off-axis angle, such that the 526 sources in the central region X-ray sample appear first, extending down to source L17 #492. The columns are (1) X-ray source number from L17, (2) and (3) optical/NIR R.A. and Decl., (4) and (5) observed 0.5-2 keV and 2-7 keV fluxes, (6) and (7) observed 850 µm flux and error, (8) a "1" if the submillimeter flux measurement is based on ALMA data and a "0" if it is based on SCUBA-2 data, (9) specz, (10) spectral class, (11) reference for the spectra used in the spectral classification (a=our Keck DEIMOS, b=Vanzella et al 2008, c,d=Balestra et al 2010, e=Szokoly et al 2004, f=Silverman et al 2010, g=Kurk et al 2013, h=Inami et al 2017, Urrutia et al 2019, i=McLure et al 2018, j=our Keck MOSFIRE, k=Kriek et al 2015, l=our Keck LRIS, m=Casey et al 2011, n=Morris et al 2015, o=Cooper et al 2012, p=Le Fèvre et al 2005, q=Mignoli et al 2005, and (12) photz from H14, or, if there is no photz in H14, then from S16. 75 · · · 53.074837 -27.787111 0.84 0.14 · · · · · · · · · · · · · · · · · · Note-The columns are (1) ALMA source number from C18, (2) X-ray source number from L17 when match exists, (3) and…”