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J/MNRAS/460/1758 Optical emission lines in galaxy cluster cores 1 (Hamer+, 2016)

Optical emission line nebulae in galaxy cluster cores 1: the morphological, kinematic and spectral properties of the sample. Hamer S.L., Edge A.C., Swinbank A.M., Wilman R.J., Combes F., Salome P., Fabian A.C., Crawford C.S., Russell H.R., Hlavacek-Larrondo J., McNamara B.R., Bremer M.N. <Mon. Not. R. Astron. Soc., 460, 1758-1789 (2016)> =2016MNRAS.460.1758H (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Redshifts Keywords: galaxies: clusters: general - galaxies: elliptical and lenticular, cD Abstract: We present an Integral Field Unit survey of 73 galaxy clusters and groups with the VIsible Multi Object Spectrograph on the Very Large Telescope. We exploit the data to determine the Hα gas dynamics on kpc scales to study the feedback processes occurring within the dense cluster cores. We determine the kinematic state of the ionized gas and show that the majority of systems (∼2/3) have relatively ordered velocity fields on kpc scales that are similar to the kinematics of rotating discs and are decoupled from the stellar kinematics of the brightest cluster galaxy. The majority of the Hα flux (>50 per cent) is typically associated with these ordered kinematics and most systems show relatively simple morphologies suggesting they have not been disturbed by a recent merger or interaction. Approximately 20 per cent of the sample (13/73) have disturbed morphologies which can typically be attributed to active galactic nuclei activity disrupting the gas. Only one system shows any evidence of an interaction with another cluster member. A spectral analysis of the gas suggests that the ionization of the gas within cluster cores is dominated by non-stellar processes, possibly originating from the intracluster medium itself. Description: This sample was drawn from the ROSAT-selected BCS (Ebeling et al., 1998, Cat. J/MNRAS/301/881) and the ESO X-ray Cluster Elliptical Spectral Survey (EXCESS) which provided long slit spectra of 201 and 446 BCGs, respectively. The EXCESS spectra were then used to identify clusters with optical line emission, the Hα emission line was identified in 30 per cent of the sample which is consistent with the findings from the BCS (Crawford et al., 1999, Cat. J/MNRAS/306/857). Only objects with an integrated Hα emission greater than 1x10-15erg/cm2/s were selected. The second selection criteria was that the Hα emission showed an extent greater than 2 arcsec in the long slit observations to ensure only objects with line emission extended on scales greater than the expected seeing were observed. The VIMOS instrument on the 8.2-m VLT was the primary optical IFU used throughout this work. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file appena.dat 123 73 The observational parameters listed for each object in the VIMOS sample (full table 1) appenf.dat 191 219 The spectroscopic properties for each object in the sample
See also: J/MNRAS/281/799 : XBACs, the sample (Ebeling+, 1996) J/MNRAS/301/881 : The ROSAT Brightest Cluster Sample. I. (Ebeling+, 1998) J/MNRAS/306/857 : The ROSAT Brightest Cluster Sample. III. (Crawford+, 1999) J/MNRAS/318/333 : Extended ROSAT Bright Cluster Sample (Ebeling+ 2000) J/A+A/425/367 : REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004) J/ApJS/182/12 : ICM entropy profiles (ACCEPT) (Cavagnolo+, 2009) Byte-by-byte Description of file: appena.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Cluster Cluster name 17- 23 F7.5 --- z Median redshift acquired from the fits to the Halpha-[NII] complex (1) 25- 33 A9 --- Grating Grating 35- 39 A5 --- Exp Total integration time on target (s) 41- 44 F4.2 arcsec Seeing ?=- Mean seeing (2) 46- 77 A32 --- Lines Lines detected (3) 79- 80 I2 h RAh Centre of the field of view Right ascension (J2000) 82- 83 I2 min RAm Centre of the field of view Right ascension (J2000) 85- 89 F5.2 s RAs Centre of the field of view Right ascension (J2000) 91 A1 --- DE- Centre of the field of view Declination sign (J2000) 92- 93 I2 deg DEd Centre of the field of view Declination (J2000) 95- 96 I2 arcmin DEm Centre of the field of view Declination (J2000) 98-102 F5.2 arcsec DEs Centre of the field of view Declination (J2000) 104-109 F6.2 10+36W LX X-ray luminosity (4) 111-115 F5.2 keV TX ?=- X-ray temperature (5) 117-123 A7 --- Class Classification (Cluster or Group1) (6)
Note (1): the median is calculated from the fits after dropping the top and bottom 2.5% of the redshifts. Note (2): The seeing is calculated as the mean of the DIMM seeing across all exposures for each object. Note (3): all lines apart from the Halpha and [NII] lines that were detected by visual inspection, the Halpha-abs line is included for systems which show some evidence of stellar Hslpha absorption. Note (4): X-ray luminosities were taken from the surveys of Bohringer et al. (2004, Cat. J/A+A/425/367); Ebeling et al. (1998, Cat. J/MNRAS/301/881; 2000, Cat. J/MNRAS/318/333) Note (5): temperatures are taken from Ebeling et al. (1996, Cat. J/MNRAS/281/799; 1998, Cat. J/MNRAS/301/881; 2000, Cat. J/MNRAS/318/333); Cavagnolo et al. (2009, Cat. J/ApJS/182/12). Note (6): The classifications are based on the X-ray properties following Bahcall (1999, Dekel A., Ostriker J.P., Formation of Structure in the Universe Cambridge Univ. Press Cambridge 135).
Byte-by-byte Description of file: appenf.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Cluster Cluster name 17- 24 A8 --- Region Region (Centre, Total or Extended) 26- 32 F7.3 10-19W/m2 [OI]1 ?=0 Line strength of [OI]lambda6300 34- 40 F7.4 10-19W/m2 e_[OI]1 ?=0 rms uncertainty on [OI]1 42- 49 F8.5 10-19W/m2 [OI]2 ?=0 Line strength of [OI]lambda6366 52- 59 F8.5 10-19W/m2 e_[OI]2 ?=0 rms uncertainty on [OI]2 61- 67 F7.3 10-19W/m2 Ha ?=0 Line strength of Hα 69- 74 F6.3 10-19W/m2 e_Ha ?=0 rms uncertainty on Ha 76- 83 F8.4 10-19W/m2 [NII] ?=0 Line strength of [NII]lambda6583 85- 91 F7.4 10-19W/m2 e_[NII] ?=0 rms uncertainty on [NII] 93-100 F8.4 10-19W/m2 [SII]1 ?=0 Line strength of [SII]lambda6716 102-108 F7.4 10-19W/m2 e_[SII]1 ?=0 rms uncertainty on [SII]1 110-117 F8.4 10-19W/m2 [SII]2 ?=0 Line strength of [SII]lambda6731 119-125 F7.4 10-19W/m2 e_[SII]2 ?=0 rms uncertainty on [SII]2 126-133 F8.5 --- [NII]/Ha ?=0 Line ratio [NII]lambda6583/Hα 135-143 F9.6 --- e_[NII]/Ha ?=0 rms uncertainty on [NII]/Ha 145-150 F6.4 --- [SII]/Ha ?=0 Line ratio [SII]lambda6716+6731/Hα 152-157 F6.4 --- e_[SII]/Ha ?=0 rms uncertainty on [SII]/Ha 159-164 F6.4 --- [OI]/Ha ?=0 Line ratio [OI]lambda6300/Hα 166-172 F7.5 --- e_[OI]/Ha ?=0 rms uncertainty on [OI]/Ha 175-181 F7.4 --- [SII]1/[SII]2 ?=0 Line ratio [SII]lambda6716/[SII]lambda6731 183-191 F9.4 --- e_[SII]1/[SII]2 ?=0 rms uncertainty on [SII]1/[SII]2
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 06-Oct-2017
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