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J/A+A/606/A12    MUSE-Wide survey: 831 emission line galaxies    (Herenz+, 2017)

The MUSE-Wide survey: A first catalogue of 831 emission line galaxies. Herenz E.C., Urrutia T., Wisotzki L., Kerutt J., Saust R., Werhahn M., Schmidt K.B., Caruana J., Diener C., Bacon R., Brinchman J., Schaye J., Maseda M., Weilbacher P.M. <Astron. Astrophys. 606, A12 (2017)> =2017A&A...606A..12H (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Galaxy catalogs ; Redshifts ; Spectroscopy Keywords: galaxies: high redshift - techniques: imaging spectroscopy - catalogs - surveys Abstract: We present a first instalment of the MUSE-Wide survey, covering an area of 22.2 arcmin2 (corresponding to ∼20% of the final survey) in the CANDELS/Deep area of the Chandra Deep Field South. We use the MUSE integral field spectrograph at the ESO VLT to conduct a full-area spectroscopic mapping at a depth of 1h exposure time per 1-arcmin2 pointing. We searched for compact emission line objects using our newly developed LSDCat software based on a 3-D matched filtering approach, followed by interactive classification and redshift measurement of the sources. Our catalogue contains 831 distinct emission line galaxies with redshifts ranging from 0.04 to 6. Roughly one third (237) of the emission line sources are Lymanα emitting galaxies with 3<z<6, only four of which had previously measured spectroscopic redshifts. At lower redshifts 351 galaxies are detected primarily by their [OII] emission line (0.3≲z≲1.5), 189 by their [OIII] line (0.21≲z≲0.85), and 46 by their Hα line (0.04≲z≲0.42). Comparing our spectroscopic redshifts to photometric redshift estimates from the literature, we find excellent agreement for z<1.5 with a median Δz of only ∼4x10-4 and an outlier rate of 6%, however a significant systematic offset of Δz=0.26 and an outlier rate of 23% for Lyα emitters at z>3. Together with the catalogue we also release 1D PSF-weighted extracted spectra and small 3D datacubes centred on each of the 831 sources. Description: This data release consists of an emission line galaxy catalogue containing 831 emission line galaxies detected in the first period of observations of the MUSE-Wide survey. We also release 1D PSF-weighted extracted spectra and 3D datacubes for each of those 831 sources. The emission line galaxy catalogue consists of two tables: A catalogue of all 831 detected emission line objects and a table of all 1652 detected emission lines in those objects. These tables are described in detail in Sect. 4.1 and 4.2 of the paper. Both tables are in the FITS binary table format, adhering to the FITS standard described in Pence et al. (2010A&A...524A..42P). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file mw1-24m.dat 142 831 Object table MW1-24main.fits 2880 49 Fits version of object table mw1-24e.dat 251 1652 Emission line table MW1-24emline.fits 2880 124 Fits version of eEmission line table spectra.dat 42 831 List of spectra 1d_spectra/* 0 831 Individual spectra 3dcubes.dat 96 831 List of datacubes 3dsourcecubes/* 0 831 Individual datacubes
See also: J/A+A/575/A75 : MUSE 3D view of HDF-S (Bacon+, 2015) J/A+A/591/A143 : NGC 3115 MUSE images (Guerou+, 2016) J/ApJ/822/78 : MACS J1149.5+2223 VLT/MUSE spectroscopic obs. (Grillo+, 2016) Byte-by-byte Description of file: mw1-24m.dat
Bytes Format Units Label Explanations
1- 9 A9 --- ID Unique MUSE-Wide object ID (UNIQUE_ID) 11- 19 F9.6 deg RAdeg Right Ascension (J2000) (RA) 21- 30 F10.6 deg DEdeg Declination (J2000) (DEC) 32- 39 F8.6 --- z Redshift of the source (Z) 41- 48 F8.6 --- e_z Error on the determined redshift (Z_ERR) 50- 53 A4 --- LeadLine Highest S/N detected line (LEAD_LINE) 55- 64 F10.5 --- SN S/N of the lead line (abbreviations according to Table 5 in the paper) (SN) 66 A1 --- Qual [abc] Quality flag (see Sect. 3.2 of the paper) (QUALITY) 68 I1 --- Conf [1/3] Confidence value (see Sect. 3.2 of the paper) (CONFIDENCE) 70-120 A51 --- OLines Other detected lines in that source (OTHER_LINES) 122-126 I5 --- GuoID ?=0 Associated source in the Guo et al. (2013, Cat. J/ApJS/207/24) photometric catalogue (Guo_ID) 128-131 F4.2 --- GuoSep ? Angular separation (in arcsec) to the Guo et al. (2013, Cat. J/ApJS/207/24) source (Guo_sep) 133-137 I5 --- SkelID ?=0 Associated source in the Skelton et al. (2014, Cat. J/ApJS/214/24) photometric catalogue (Skelton_ID) 139-142 F4.2 --- SkelSep ? Angular separation to the Skelton et al. (2014, Cat. J/ApJS/214/24) source (Skelton_sep)
Byte-by-byte Description of file: mw1-24e.dat
Bytes Format Units Label Explanations
1- 9 A9 --- ID Unique MUSE-Wide object ID (UNIQUE_ID) 11- 12 I2 --- PointID MUSE-Wide Pointing ID (see Fig. 1 in paper) (POINTING_ID) 14- 15 I2 --- ObjID Object ID (only unique per pointing) (OBJ_ID) 17- 19 I3 --- RID Running ID (only unique per pointing) (RID) 21- 24 A4 --- Ident Line identification (abbreviations according to Table 5 in the paper) (IDENT) 26- 52 A27 --- ( Com$ Comment (COMMENT) (1) 54- 63 F10.5 --- SN Detection significance (SN) 65- 73 F9.6 deg RAdeg 3D S/N weighted emission line position in datacube (right ascension, J2000) (RA_SN) 75- 84 F10.6 deg DEdeg 3D S/N weighted emission line position in datacube (declination J2000) (DEC_SN) 86- 93 F8.3 0.1nm lambda 3D S/N weighted emission line air wavelength in datacube (LAMBDA_SN) 95-103 F9.6 deg RApdeg 3D S/N peak emission line position in datacube (right ascension J2000) (RAPEAKSN) 105-114 F10.6 deg DEpdeg 3D S/N peak emission line position in datacube (declination J2000) (DECPEAKSN) 116-123 F8.3 0.1nm lambdap 3D S/N peak emission line air wavelength in datacube (LAMBDAPEAKSN) 125-132 F8.3 0.1nm b_lambdaNB Lower value of lambdaNB interval (LAMBDANBMIN) 134-141 F8.3 0.1nm B_lambdaNB Upper value of lambdaNB interval (LAMBDANBMAX) 143-151 F9.6 deg RA1deg First central moment position of emission line, right ascension J2000 (RA_1MOM) (2) 153-162 F10.6 deg DE1deg First central moment position of emission line, declination J2000 (DEC_1MOM) (2) 164-171 F8.6 arcsec RKron Kron radius (R_KRON) (3) 173-181 F9.3 mW/m2 FKron Emission line flux extracted in RKron radius aperture (F_KRON) (3) 183-192 F10.3 mW/m2 F2Kron Emission line flux extracted in 2RKron radius aperture (F_2KRON) (3) 194-203 F10.3 mW/m2 F3Kron Emission line flux extracted in 3RKron radius aperture (F_3KRON) (3) 205-214 F10.3 mW/m2 F4Kron Emission line flux extracted in 4RKron radius aperture (F_4KRON) 216-222 F7.3 mW/m2 e_FKron rms uncertainty on FKron (FKRONERR) 224-231 F8.3 mW/m2 e_F2Kron rms uncertainty on F2Kron (F2KRONERR) 233-240 F8.3 mW/m2 e_F3Kron rms uncertainty on F3Kron (F3KRONERR) 242-249 F8.3 mW/m2 e_F4Kron rms uncertainty on F4Kron (F4KRONERR) 251 I1 --- Border [0,1] Flag indicating whether 3*R_KRON overlaps with pointing border (BORDER_FLAG)
Note (1): added during classifications and cleaning (see Sect. 3.2 in the paper) Note (2): see Sect. 3.3 in the paper. Note (3): Kron radius (Kron, 1980ApJS...43..305K)
Byte-by-byte Description of file: spectra.dat
Bytes Format Units Label Explanations
1- 9 I9 --- ID Unique MUSE-Wide object ID 11- 14 I4 --- Nx Number of pixels along X-axis 16- 18 I3 Kibyte size Size of FITS file 20- 42 A23 --- FileName Name of FITS file, in subdirectory 1d_spectra (1)
Note (1): The 1D spectra are in the sub-directory 1d_spectra and have the filenames spectrum_NNNNNNNNN.fits, where NNNNNNNNN refers to the objects MUSE-Wide UNIQUE_ID. The 1D spectra are provided as FITS binary tables (Pence et al., 2010A&A...524A..42P) with 4 columns: (1) WAVE_AIR: Air wavelength (in Angstroem). (2) WAVE_VAC: Vacuum wavelength (in Angstroem). Converted from air wavelength with the formula used in the Vienna atomic line database (Ryabchikova et al., 2015, Phys. Scr., 90, 054005): http://www.astro.uu.se/valdwiki/Air-to-vacuum%20conversion (3) FLUX: Flux density for a given wavelength bin (in 10-20erg/s/cm2/Angstroem) (4) FLUX_ERR: Error on the flux density in column (3) (in 10-20erg/s/cm2/Angstroem)
Byte-by-byte Description of file: 3dcubes.dat
Bytes Format Units Label Explanations
1- 9 I9 --- ID Unique MUSE-Wide object ID 11- 19 F9.5 deg RAdeg Right Ascension of center (J2000) 20- 28 F9.5 deg DEdeg Declination of center (J2000) 30- 32 F3.1 arcsec/pix scale Scale of the image 34- 36 I3 --- Nx Number of pixels along X-axis 38- 40 I3 --- Ny Number of pixels along Y-axis 42- 45 I4 --- Nz Number of slices 47- 53 F7.2 0.1nm blambda Lower value of wavelength interval 55- 61 F7.2 0.1nm Blambda Upper value of wavelength interval 63- 66 F4.2 0.1nm dlambda Wavelength resolution 68- 73 I6 Kibyte size Size of FITS file 75- 96 A22 --- FileName Name of FITS file, in subdirectory 3dsourcecubes (1)
Note (1): The 3D source datacubes are in the sub directory 3dsourcecubes, with filenames NNNNNNNNN_objcube.fits, where NNNNNNNNN refers to the objects MUSE-Wide UNIQUE_ID. These FITS files consist of 3 header-data units, with correct world-coordinates included in each header following the conventions given in Calabretta & Greisen (2002A&A...395.1077C), Greisen & Calabretta (2002A&A...395.1061G), and Greisen et al. (2006A&A...446..747G). (HDU 1): A datacube of dimensions a*b*3680, where a and b are the spatial dimensions matched to the objects extent, and 3680 is the spectral dimension. Each volume pixel stores the flux density in 10-20erg/s/cm2/Angstroem. (HDU 2): A vector of length 3680 storing the variance for each wavelength layer in the datacube. (HDU 3): An array of dimensions a*b storing the amount of MUSE exposures that went into each spectral pixel of the datacube.
Acknowledgements: Christian Herenz, christian.herenz(at)astro.su.se
(End) Patricia Vannier [CDS] 23-May-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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