J/A+A/629/A102 Halpha data cube of Stephan's Quintet (Duarte Puertas+, 2019)
Searching for intergalactic star forming regions in Stephan's Quintet with
SITELLE. I. Ionised gas structures and kinematics.
Duarte Puertas S., Iglesias-Paramo J., Vilchez J.M., Drissen L., Kehrig C.,
Martin T.
<Astron. Astrophys. 629, A102 (2019)>
=2019A&A...629A.102D 2019A&A...629A.102D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, optical ; Photometry, H-alpha
Keywords: galaxies: evolution - galaxies: groups: general -
galaxies: kinematics and dynamics - galaxies: star formation
Abstract:
Stephan's Quintet (SQ), the prototypical compact group of galaxies in
the local Universe, has been observed with the imaging Fourier
transform spectrometer SITELLE, attached to the Canada-France-Hawaii-
Telescope, to perform a deep search for intergalactic star-forming
emission. In this paper we present the extended ionised gaseous
structures detected and analyse their kinematical properties. The
large field of view (11'x11') and the spectral ranges of SITELLE have
allowed a thorough study of the entire galaxy system, its interaction
history and the main properties of the ionised gas. The observations
have revealed complex three-dimensional strands in SQ seen for the
first time, as well as the spatially resolved velocity field for a new
SQ dwarf galaxy (M82-like) and the detailed spectral map of NGC7320c,
confirming its AGN nature. A total of 175 SQ Halpha emission regions
have been found, 22 of which present line profiles with at least two
kinematical components. We studied 12 zones and 28 sub-zones in the SQ
system in order to define plausible physical spatial connections
between its different parts in the light of the kinematical
information gathered. In this respect we have found five velocity
systems in SQ: i) v=[5600-5900]km/s associated with the new intruder
and the southern debris region; ii) v=[5900-6100]km/s, associated with
the north starburst A and south starburst A and the strands connected
to these zones; iii) v=[6100-6600]km/s, associated with the strands
from the large-scale shock region (LSSR); iv) v=[6600-6800]km/s,
associated with the young tidal tail, the starburst A (SQA), NGC7319,
and the NGC7319 north lobe; and v) v=[6800-7000]km/s, associated with
the strands seen connecting LSSR with SQA. We fail to detect ionised
gas emission in the old tail, neither in the vicinity of NGC7318A nor
in NGC7317, and the connection between NGC7319 north lobe and SQA
cannot be confirmed. Conversely, a clear gaseous bridge has been
confirmed both spatially and kinematically between the LSSR zone and
the NGC7319 AGN nucleus. Finally, a larger scale, outer rim winding
the NGC7318B/A system clockwise north-west to south-east has been
highlighted in continuum and in Hα. This structure may be
reminiscent of a sequence of a previously proposed scenario for SQ a
sequence of individual interactions.
Description:
Halpha flux datacube in FITS format for all the SQ compact group. The
units of the Halpha flux are erg/s/cm2. The data were fitted using
the Python-based software ORCS (Martin et al., 2015, in Astronomical
Society of the Pacific Conference Series, Vol. 495, Astronomical Data
Analysis Software an Systems XXIV (ADASS XXIV), ed. A. R. Taylor & E.
Rosolowsky, 327). The observing parameters and data reduction of SQ
are described in the paper. This reduced data cube is made according
to Fig. 3 in the paper (see Sect. 2.2.2.). This figure shows the
Halpha flux and Halpha radial velocity maps for all the pixels
(binning 3x3) found in SQ with contrast(Halpha) higher or equal than 5
in the radial velocity range [5400, 7050]km/s. We fitted each spectrum
to a sincgauss function for Hα and [NII]6548,6583 simultaneously
using only one velocity component; the complex kinematics spectral
fitting of emission regions cannot be considered in this datacubes.
Positions of the SQ Halpha emission regions are shown in Table B, see
the paper for details.
Objects:
------------------------------------------------------
RA (2000) DE Designation(s)
------------------------------------------------------
22 35 57.5 +33 57 36 Stephan's Quintet = HCG 92
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File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
list.dat 118 1 Information of datacube
fits/* . 1 Datacube
--------------------------------------------------------------------------------
Byte-by-byte Description of file: list.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
11- 19 F9.5 deg DEdeg Declination of center (J2000)
21- 24 F4.2 arcsec/pix Scale Scale of the image
26 I1 --- Binning Binning
28- 31 I4 --- Nx Number of pixels along X-axis
33- 36 I4 --- Ny Number of pixels along Y-axis
38- 39 I2 --- Nz Number of slices
41- 50 A10 "date" Date Observation date
52- 55 I4 km/s bVELO-HEL Lower value of velocity interval
57- 60 I4 km/s BVELO-HEL Upper value of velocity interval
62- 63 I2 km/s dVELO-HEL Velocity resolution
65- 71 I7 Kibyte size Size of FITS file
73- 83 A11 --- FileName Name of FITS file, in subdirectory fits
85-118 A34 --- Title Title of the FITS file
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History:
From Salvador Duarte Puertas, salvini(at)iaa.es
Acknowledgements:
We thank the anonymous referee for very constructive suggestions that
have improved this manuscript. Based on observations obtained with
SITELLE, a joint project of Universite Laval, ABB, Universite de
Montreal, and the Canada-France-Hawaii Telescope (CFHT), which is
operated by the National Research Council of Canada, the Institut
National des Sciences de l'Univers of the Centre National de la
Recherche Scientifique of France, and the University of Hawaii. The
authors wish to recognise and acknowledge the very significant
cultural role that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most grateful to have the
opportunity to conduct observations from this mountain. SDP, JIP, JVM,
and CK acknowledge financial support from the Spanish Ministerio de
Economia y Competitividad under grants AYA2013-47742-C4-1-P and
AYA2016-79724-C4-4-P, from Junta de Andalucia Excellence Project
PEX2011-FQM-7058, and also acknowledge support from the State Agency
for Research of the Spanish MCIU through the 'Center of Excellence
Severo Ochoa' award for the Instituto de Astrofisica de Andalucia
(SEV-2017-0709). LD is grateful to the Natural Sciences and
Engineering Research Council of Canada, the Fonds de Recherche du
Quebec, and the Canada Foundation for Innovation for funding. This
research made use of Python (http://www.python.org) and IPython
(Perez & Granger, 2007, Computing in Science and Engineering, 9, 21);
Numpy (Van Der Walt et al., 2011, ArXiv e-prints); Pandas (McKinney,
2010, in Proceedings of the 9th Python in Science Conference, ed. S.
van der Walt & J. Millman, 51-56); of Matplotlib (Hunter, 2007,
Computing In Science & Engineering, 9, 90), a suite of open-source
Python modules that provides a framework for creating scientific
plots. This research made use of Astropy, a community-developed core
Python package for Astronomy (Astropy Collaboration et al.,
2013A&A...558A..33A 2013A&A...558A..33A). The Astropy web site is http://www.astropy.org.
This research made use of astrodendro, a Python package to compute
dendrograms of astronomical data (http://www.dendrograms.org/).
(End) Patricia Vannier [CDS] 09-Sep-2019