J/A+A/667/A141 Hubble Asteroid Hunter. II. (Garvin+, 2022)
Hubble Asteroid Hunter.
II. Identifying strong gravitational lenses in HST images with crowdsourcing.
Garvin E.O., Kruk S., Cornen C., Bhatawdekar R., Canameras R., Merin B.
<Astron. Astrophys. 667, A141 (2022)>
=2022A&A...667A.141G 2022A&A...667A.141G (SIMBAD/NED BibCode)
ADC_Keywords: Gravitational lensing ; Galaxy catalogs
Keywords: gravitational lensing: strong - catalogs - galaxies: general -
Abstract:
The Hubble Space Telescope (HST) archives constitute a rich dataset of
high-resolution images to mine for strong gravitational lenses. While
many HST programmes specifically target strong lenses, they can also
be present by coincidence in other HST observations.
Our aim is to identify non-targeted strong gravitational lenses,
without any prior selection on the lens properties, in almost two
decades of images from the ESA Hubble Space Telescope archive (eHST).
We used crowdsourcing on the Hubble Asteroid Hunter (HAH) citizen
science project to identify strong lenses, along with asteroid trails,
in publicly available large field-of-view HST images. We visually
inspected 2 354 objects tagged by citizen scientists as strong lenses
to clean the sample and identify the genuine lenses.
We report the detection of 252 strong gravitational lens candidates,
which were not the primary targets of the HST observations. A total of
198 of them are new, not previously reported by other studies,
consisting of 45 A grades, 74 B grades and 79 C grades. The majority
are galaxy-galaxy configurations. The newly detected lenses are, on
average, 1.3 magnitudes fainter than previous HST searches. This
sample of strong lenses with high-resolution HST imaging is ideal to
follow up with spectroscopy for lens modelling and scientific
analyses.
This paper presents the unbiased search of lenses that enabled us to
find a wide variety of lens configurations, including exotic lenses.
We demonstrate the power of crowdsourcing in visually identifying
strong lenses and the benefits of exploring large archival datasets.
This study shows the potential of using crowdsourcing in combination
with artificial intelligence for the detection and validation of
strong lenses in future large-scale surveys such as ESA's Euclid
mission or in JamesWebb Space Telescope (JWST) archival images.
Description:
We present a sample of 252 strong gravitational lenses found by
citizen scientists from the Hubble Asteroid Hunter crowdsourcing
project, in HST archives covering almost two decades of observations.
This table groups the data presented in Tables A.1, A.2 and A.3 in the
Appendix of the paper. It summarizes the characteristics of each of
the 198 discovered and 54 rediscovered lens objects (Tables A.1. and
A.2. respectively), such as the IAU name of the lens object, the
existence of a group scale, the ID of the lensing system as presented
in the paper, the coordinates (ra, dec), the arc radius, the
instrument and filter, the Galfit parameters (mag, re, q, pa), the
class of the source images, and the redshift. If the lens is a new
discovery (c.f. Table A.1.) the proposal ID is provided, while if if
is a rediscovery (c.f. Table A.2.) the corresponding paper is cited.
Finally, it provides detailed indications of the possible presence of
a nearby cluster based on cluster catalogues crossmatches, as
presented in Table A.3.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea.dat 224 270 Gravitational lenses identified in the
Hubble Space Telescope observation (tables A1-A3)
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See also:
J/A+A/661/A85 : Asteroid trails in HST images (Kruk+, 2022)
Byte-by-byte Description of file: tablea.dat
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Bytes Format Units Label Explanations
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1- 22 A22 --- Name IAU Name: Hubble Asteroid Hunter
(HAH JHHMMSS.s+DDMMSS.s)
24- 26 A3 --- GroupScale [yes/no ] Indicates if the object is believed
to be the member of a group scale (1)
27- 30 I4 --- ID Internal lens ID from the paper, (2)
32 A1 --- Grade [ABC] The grade of the lens assigned by
the authors (3)
34- 42 F9.5 deg RAdeg Right ascension (J2000)
44- 52 F9.5 deg DEdeg Declination (J2000)
54- 58 F5.3 arcsec rarc ?=- Arc radius indicating the angular
separation between the lens and the image
of the source
60- 68 A9 --- Inst HST instrument and aperture
(ACS/WFC3, WFC3/UVIS or WFC3/IR)
70- 75 A6 --- Filt HST filter in which the lens was discovered
and fitted with GALFIT
77- 80 F4.1 mag mag ?=- Magnitude of the lens
(measured with GALFIT)
82- 86 F5.2 arcsec re ?=- Effective radius of the lens
(measured with GALFIT)
88- 91 F4.2 --- q ?=- Axis ratio of the lens
(measured with GALFIT)
93- 98 F6.1 deg PA []?=- Position angle of the lens
(measured with GALFIT), measured from North
through East
100-105 A6 --- Class The morphological class of the source images,
with the following categories:
Arc, Ring, Quad, Double, Triple, Cross
107-110 F4.2 --- z ?=- Redshift of the lens
111 A1 --- r_z [*] * indicates retrieved either from NED
or from SDSS
112 A1 --- n_z [SP] "S" indicates spectroscopic redshift,
"P" is the photometric redshift
114-118 I5 --- PropID ?=- The ID of the HST proposal in which the
serendipitous strong lens was found (4)
120-142 A23 --- Ref Reference to the article in which the lens
was first reported (5)
144-170 A27 --- Target Name of the HST observation target in which
the lens was found, if the target was a
galaxy cluster
171-180 I10 --- DESI ?=- ID of candidate galaxy cluster from DESI
(Zou et al, 2021, Cat. J/ApJS/253/56) found
within 3 arcmin from the gravitational lens
182-191 F10.6 arcsec Ddesi ?=- Angular distance from the lens to the
DESI cluster
194-213 A20 --- RedMap ID of candidate galaxy cluster from SDSS
RedMaPPer (Rykoff et al., Cat. J/ApJ/785/104)
found within 3 arcmin from the
gravitational lens
215-224 F10.6 arcsec Dredmap ? Angular distance from the lens to the
RedMaPPer cluster
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Note (1): If the object is part of a group scale (i.e. a group of galaxies
acting as a unique lensing system), it will present one row per galaxy.
The parameters which relate to the system will be shared and identical to those
of other members of the group scale (id, grade, ra, dec, rarc, instr, filter,
class, z and clusters), and some parameters will be specific to the galaxy
(mag, re, q, pa).
Note (2): Group scale lenses share the same ID as the member galaxies are
considered as a unique lens system. We have 252 IDs representing unique lensing
systems, while the table contains 270 row entries as the group scales are
constituted of one system with several galaxies (and hence several row
entries).
Note (3): grade as follows:
A = almost certainly a lens
B = highly probable lens
C = maybe a lens
Note (4): The lenses presented in the paper were not the target of the
observation.
Note (5): References as follows:
Bettoni et al. 2019 = 2019ApJ...873L..14B 2019ApJ...873L..14B
Brownstein et al. 2012 = 2012ApJ...744...41B 2012ApJ...744...41B
Cabanac et al. 2007 = 2007A&A...461..813C 2007A&A...461..813C
Clowe et al. 2012 = 2012ApJ...758..128C 2012ApJ...758..128C
Desprez et al. 2018 = 2018MNRAS.479.2630D 2018MNRAS.479.2630D
Diego et al. 2015 = 2015MNRAS.449..588D 2015MNRAS.449..588D
Ebeling et al. 2014 = 2014ApJS..211...21E 2014ApJS..211...21E, Cat. J/ApJS/211/21
Ebeling et al. 2018 = 2018ApJ...852L...7E 2018ApJ...852L...7E
Ebeling et al. 2019 = 2019hst..prop15843E
Fassnacht et al. 2004 = 2004ApJ...600L.155F 2004ApJ...600L.155F, Cat. J/ApJ/600/L155
Faure et al. 2008 = 2008ApJS..176...19F 2008ApJS..176...19F, Cat. J/ApJS/176/19
Fort et al. 1992 = 1992ApJ...399L.125F 1992ApJ...399L.125F
Grillo et al. 2008 = 2008A&A...486...45G 2008A&A...486...45G
Guzzo et al. 2009 = 2009A&A...499..357G 2009A&A...499..357G, Cat. J/A+A/499/357
Horesh et al. 2010 = 2010MNRAS.406.1318H 2010MNRAS.406.1318H, Cat. J/MNRAS/406/1318
Jackson 2008 = 2008MNRAS.389.1311J 2008MNRAS.389.1311J
Jacobs et al. 2019 = 2019ApJS..243...17J 2019ApJS..243...17J, Cat. J/ApJS/243/17
Koester et al. 2010 = 2010ApJ...723L..73K 2010ApJ...723L..73K
Lagattuta et al. 2010 = 2010ApJ...716.1579L 2010ApJ...716.1579L
Marshall et al. 2009 = 2009ApJ...694..924M 2009ApJ...694..924M
More et al. 2011 = 2011ApJ...734...69M 2011ApJ...734...69M
More et al. 2012 = 2012ApJ...749...38M 2012ApJ...749...38M, Cat. J/ApJ/749/38
Morishita et al. 2017 = 2017ApJ...835..254M 2017ApJ...835..254M, Cat. J/ApJ/835/254
Moustakas et al. 2007 = 2007ApJ...660L..31M 2007ApJ...660L..31M
Pawase et al. 2014 = 2014MNRAS.439.3392P 2014MNRAS.439.3392P
Pourrahmani et al. 2018 = 2018ApJ...856...68P 2018ApJ...856...68P, Cat. J/ApJ/856/68
Ragozzine et al. 2012 = 2012ApJ...744...94R 2012ApJ...744...94R
Rattunga et al. 1995 = 1995ApJ...453L...5R 1995ApJ...453L...5R
Repp et al. 2018 = 2018MNRAS.479..844R 2018MNRAS.479..844R
Richard et al. 2015 = 2015MNRAS.446L..16R 2015MNRAS.446L..16R
Schirmer et al. 2010 = 2010A&A...514A..60S 2010A&A...514A..60S, Cat. J/A+A/514/A60
Sharon et al. 2020 = 2020ApJS..247...12S 2020ApJS..247...12S, Cat. J/ApJS/247/12
Smail et al. 2007 = 2007ApJ...654L..33S 2007ApJ...654L..33S
Zitrin et al. 2015 = 2015ApJ...801...44Z 2015ApJ...801...44Z, Cat. J/ApJ/801/44
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Acknowledgements:
Emily Garvin, egarvin(at)phys.ethz.ch
References:
Kruk et al., Paper I 2022A&A...661A..85K 2022A&A...661A..85K, Cat. J/A+A/661/A85
(End) Patricia Vannier [CDS] 21-Oct-2022