J/MNRAS/533/4334 SAMI Galaxy Survey: detailed classifications (Tuntipong+, 2024)
The SAMI galaxy survey: on the importance of applying multiple selection
criteria for finding Milky Way analogues.
Tuntipong S., van de Sande J., Croom S.M., Barsanti S., Bland-Hawthorn J.,
Brough S., Bryant J.J., Casura S., Fraser-McKelvie A., Lawrence J.S.,
Ristea A., Sweet S.M., Zafar T.
<Mon. Not. R. Astron. Soc., 533, 4334-4359 (2024)>
=2024MNRAS.533.4334T 2024MNRAS.533.4334T (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Galaxy catalogs ; Morphology ; Galaxies, nearby ;
Galaxies, optical
Keywords: surveys - galaxies: clusters: general - galaxies: general -
galaxies: kinematics and dynamics - galaxies: star formation
Abstract:
Milky Way analogues (MWAs) provide an alternative insight into the
various pathways that lead to the formation of disc galaxies with
similar properties to the Milky Way (MW). In this study, we explore
different selection techniques for identifying MWAs in the Sydney-AAO
(Australian Astronomical Observatory) Multi-object Integral field
spectrograph (SAMI) Galaxy Survey. We utilize a nearest neighbours
method to define MWAs using four selection parameters including
stellar mass (M*), star formation rate (SFR), bulge-to-total ratio
(B/T), and disc effective radius (Re). Based on 15 different selection
combinations, we find that including M* and SFR is essential for
minimizing biases in the average MWA properties as compared to the MW.
Furthermore, given the MW's smaller than average size, selection
combinations without Re result in MWAs being too large. Lastly, we
find that B/T is the least important parameter out of the four tested
parameters. Using all four selection criteria, we define the top 10
most MW-like galaxies in the GAMA and Cluster regions of the SAMI
survey. These most MW-like galaxies are typically barred spirals, with
kinematically cold rotating discs and reside in a wide range of
environments. Surprisingly, we find no significant differences between
the MWAs selected from the GAMA and Cluster regions. Our work
highlights the importance of using multiple selection criteria for
finding MWAs and also demonstrates potential biases in previous MWA
studies.
Description:
The SAMI Galaxy survey observations were carried out between 2013 and
2018, which resulted in over 3000 unique galaxies being observed
across a wide range of mass and environments with spatially resolved
structural and kinematics measurements. Hubble-style morphological
classifications of SAMI galaxies presented in Cortese et al.
(2016MNRAS.463..170C 2016MNRAS.463..170C), and this catalogue builds on this previous work
by supplying detailed morphological classifications for the same SAMI
sample. In particular, we aimed to classify bars, tidal interactions,
and other less common features. All SAMI galaxies were visually
classified and inspected for bars and signs of interaction. The visual
classification was performed on colour images from three surveys:
Hyper Suprime-Cam (HSC), the Dark Energy Camera Legacy Survey (DECaLS)
or the Panoramic Survey Telescope and Rapid Response System
(Pan-STARRS). All available imaging for a given galaxy was presented
to the classifier, and so classifiers viewed between one and three
images of a given galaxy before deciding on a classification. The
classification was performed by 3 or 4 contributors, except 305
galaxies in APMCC 917, Abell 4038, EDCC 442, and Abell 3880 that were
classified by AFM. The best image quality was from HSC (FWHM=0.67"),
followed by DeCaLS (FWHM=1.11"), and Pan-STARRS (FWHM=1.30"). We note
that HSC imaging was not available for all galaxies. We required a
minimum classification fraction of 1/3 to indicate the presence of a
bar or signs of interactions.
This catalogue was generated on 8 October 2021 by Amelia
Fraser-McKelvie, with the help of classifications from Angel
Lopez-Sanchez, Darren Croton, Duncan Forbes, Giulia Santucci, James
Agostino, James Pinto Correia, Jesse van de Sande, Kate Harborne, Luca
Cortese, Mina Pak, Richard McDermid + his students, Sarah Brough,Sarah
Caesura, Sarah Leslie, Sarah Sweet, Scott Croom, Sree Oh, Stefania
Barsanti and Tom Rutherford.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
samicat.dat 364 3070 SAMI detailed classifications
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See also:
J/MNRAS/446/1567 : SAMI Galaxy Survey: EDR (Allen+, 2015)
http://sami-survey.org/ : SAMI Galaxy Survey Home Page
Byte-by-byte Description of file: samicat.dat
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Bytes Format Units Label Explanations
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1- 10 I10 --- SAMI SAMI CATID (CATID_EXT)
12- 29 F18.14 deg RAdeg Right Ascension (J2000) of object
(RA_OBJ)
31- 51 F21.17 deg DEdeg Declination (J2000) of object (DEC_OBJ)
53- 73 F21.19 --- zsp Spectroscopic redshift (z_spec)
75- 92 F18.16 --- fstrong-bar [0/1] Fraction of respondents that
classified this galaxy as having a
strong bar (strongbarfract)
94-111 F18.16 --- fweak-bar [0/1] Fraction of respondents that
classified this galaxy as having a
weak bar (weakbarfract)
113-130 F18.16 --- ftot-bar [0/1] Fraction of respondents that
classified this galaxy as having any
type of bar
(= strongbarfract + weakbarfract)
(totbarfract)
132-149 F18.16 --- fBP-bulge [0/1] Fraction of respondents that
classified this galaxy as having a
boxy-peanut bulge (BPbulgefract)
151-168 F18.16 --- fLSB-comp [0/1] Fraction of respondents that
classified this galaxy as having a low
surface- brightness companion
(LSBcompanionfract)
170-187 F18.16 --- fmerger [0/1] Fraction of respondents that
classified this galaxy as having a
merger (two systems that are very close
to one another such that they are
basically one system now)
(merger_fract)
189-206 F18.16 --- finter [0/1] Fraction of respondents that
classified this galaxy as undergoing
an interaction including tidal tails
(galaxy shows signs of disturbance but
is still considered a separate galaxy)
(interaction_fract)
208-225 F18.16 --- fshells-or-asym [0/1] Fraction of respondents that
classified this galaxy as having shells
or asymmetry (incl merger remnants)
(shellsorasymmetry_fract)
227-244 F18.16 --- fany-inter [0/1] Fraction of respondents that
classified this galaxy as having any
evidence for an interaction (incl
merger, tidal tails, asymmetry, or
shells). (= merger_fract +
interaction_fract +
shellsorasymmetry_fract, Max=1])
(anyinteractionfract)
246-364 A119 --- Com Any comments left by classifiers
(comments)
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Acknowledgements:
Amelia Fraser-McKelvie, Amelia.Fraser-McKelvie(at)eso.org
Sujeeporn Tuntipong, stun4076(at)uni.sydney.edu.au
References:
Croom et al., 2021MNRAS.505..991C 2021MNRAS.505..991C,
The SAMI Galaxy Survey: the third and final data release
Miyazaki et al., 2018PASJ...70S...1M 2018PASJ...70S...1M,
Hyper Suprime-Cam: System design and verification of image quality
Flewelling et al., 2020ApJS..251....7F 2020ApJS..251....7F,
The Pan-STARRS1 Database and Data Products
Dey et al., 2019AJ....157..168D 2019AJ....157..168D,
Overview of the DESI Legacy Imaging Surveys
(End) Sujeeporn Tuntipong [USyd, Australia], Patricia Vannier [CDS] 12-Oct-2024