J/MNRAS/522/173 HST colors of ESO 137-001 tail stars (Waldron+, 2023)
HST viewing of spectacular star-forming trails behind ESO 137-001.
Waldron W., Sun M., Luo R., Laudari S., Chatzikos M., Sivanandam S.,
Kenney J.D.P., Jachym P., Voit G.M., Donahue M., Fossati M.
<Mon. Not. R. Astron. Soc. 522, 173-194 (2023)>
=2023MNRAS.522..173W 2023MNRAS.522..173W (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Star Forming Region ; H II regions ; YSOs ;
Positional data ; Photometry, HST ; Ultraviolet ; Optical ;
Infrared
Keywords: galaxies: clusters: individual: Abell 3627 - galaxies: evolution -
galaxies: individual: (ESO 137-001) - galaxies: starburst -
galaxies: star formation
Abstract:
We present the results from the HST WFC3 and ACS data on an archetypal
galaxy undergoing ram pressure stripping (RPS), ESO 137-001, in the
nearby cluster Abell 3627. ESO 137-001 is known to host a prominent
stripped tail detected in many bands from X-rays, H α to CO. The
HST data reveal significant features indicative of RPS such as
asymmetric dust distribution and surface brightness as well as many
blue young star complexes in the tail. We study the correlation
between the blue young star complexes from HST, H II regions from H
α (MUSE), and dense molecular clouds from CO (ALMA). The
correlation between the HST blue star clusters and the H II regions is
very good, while their correlation with the dense CO clumps are
typically not good, presumably due in part to evolutionary effects. In
comparison to the STARBURST99 + CLOUDY model, many blue regions are
found to be young (<10 Myr) and the total star formation (SF) rate in
the tail is 0.3-0.6 M☉/yr for sources measured with ages less
than 100 Myr, about 40 per cent of the SF rate in the galaxy. We trace
SF over at least 100 Myr and give a full picture of the recent SF
history in the tail. We also demonstrate the importance of including
nebular emissions and a nebular to stellar extinction correction
factor when comparing the model to the broad-band data. Our work on
ESO 137-001 demonstrates the importance of HST data for constraining
the SF history in stripped tails.
Description:
It has been long known that the environments where galaxies reside
affect their properties and evolution. Galaxies can be shaped by
gravitational processes, e.g. mergers and tidal stripping. Another
important process that shapes galaxies, especially in galaxy clusters
and groups, is ram pressure stripping. ESO 137-001 a spiral galaxy
near the centre of the closest rich cluster, the Norma cluster (Abell
3627), was first discovered as a galaxy undergoing RPS) with the
Chandra and XMM X-ray data. Many outstanding questions remain, e.g.
the impact of RPS on galaxy properties, the star formation (SF)
efficiency in tails, roles of magnetic field and turbulence, and the
spatial and kinematic connection for gas of different phases. To
address these questions, a multiwavelength approach is required. Among
all the multiwavelength data, optical/UV broad-band data with HST
present the sharpest view of SF in the stripped tails and allow
detailed constraints on the sink term of the multiphase stripped
tails. ESO 137-001 has become the RPS galaxy with the richest amount
of supporting data and multiwavelength analysis (MUSE, HST, ALMA,
Spitzer Chandra, XMM).
This work presents this type of study with the Hubble Space Telescope
(HST) data, on the archetypal RPS galaxy, ESO 137-001, also the one
with the brightest diffuse H α tail and the richest amount of
multiwavelength supporting data . It is also the only RPS galaxy in
the JWST GTO program with 14.5 h. Here, we study the impact of RPS
on the galaxy. We intend to quantify the star formation rate (SFR) in
the tail and compare the HST results with those from H α
observations. The SFR history in the tail is also examined, as well as
connection between young star clusters/complexes, H II, regions, and
CO clouds. Concerning HST data, we focus on WFC3 and ACS especially
with HST WFC3 UVIS and HST WFC3 IR to acquire F275W, F475W and F814W
apparent magnitudes and colors.
Next, as explained in section 4, regions of interest and source sample
on mainly young star complexes in ESO 137-1 tail, the HST photometry
studies of individual sources, the baseline sample of sources as
sources covered by the F275W, F475W, and F814W data. Selection
criteria is defined on colors values and data quality. It gives rise
the source number to 520. This final sample includes 127 in the H II
regions, 201 in the tail, 140 in the galaxy and 36 in the control
region. The sources defined in the baseline sample are shown in Fig. 6
of the section 4.1 which presents the sources identified in the H II
regions in red and other sources identified within the tail. Their HST
photometric and astrometric data are presented in tablea1.dat.
Objects:
----------------------------------------------------------------------------
RA (2000) DE Designation(s)
----------------------------------------------------------------------------
16 14 22.49 -60 52 06.9 ACO 3627 = NAME Norma Cluster
16 13 27.30 -60 45 50.5 ESO 137-1 = 2MASX J16132730-6045505
----------------------------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 61 504 HST magnitudes and colors of individual sources
in ESO 137-001 tail structure
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See also:
J/MNRAS/428/1880 : Far-IR properties of VCC galaxies (Auld+, 2013)
J/MNRAS/419/3505 : The HeViCS Bright Galaxy Sample (Davies+, 2012)
J/A+A/537/A146 : Stellar models with rotation. 0.8<M<120, Z=0.014
(Ekstrom+, 2012)
J/A+A/415/9 : Redshifts behind the Southern Milky Way (Woudt+, 2004)
J/ApJ/923/278 : Massive star cluster in LIRGs in GOALS. II. (Linden+, 2021)
J/ApJS/191/143 : HST/ACS Coma cluster survey. II. (Hammer+, 2010)
J/AJ/163/16 : Multiwavelength study in M33 star clusters (Moeller+, 2022)
I/305 : The Guide Star Catalog, Version 2.3.2 (GSC2.3)
(STScI, 2006)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- ID Identifier raw number (IDNumber)
5- 6 I2 h RAh Right ascension (J2000)
8- 9 I2 min RAm Right ascension (J2000)
11- 15 F5.2 s RAs Right ascension (J2000)
17 A1 --- DE- Declination sign (J2000)
18- 19 I2 deg DEd Declination (J2000)
21- 22 I2 arcmin DEm Declination (J2000)
24- 28 F5.2 arcsec DEs Declination (J2000)
30- 34 F5.2 mag F475W The HST F475W apparent magnitude centered
on 475nm (F475W)
36- 39 F4.2 mag e_F475W Uncertainty of F475W (errF475W)
41- 45 F5.2 mag F275W-F475W Apparent color HST magnitude F275W-F475W
centered respectively on 275 nm and 475nm
(F275W-F475W)
47- 50 F4.2 mag e_F275W-F475W Uncertainty of F275W-F475W
(errF275W-F475W)
52- 56 F5.2 mag F475W-F814W Apparent color HST magnitude F475W-F814W
centered respectively on 475nm and 814nm
(F475W-F814W)
58- 61 F4.2 mag e_F475W-F814W Uncertainty of F475W-F814W
(errF475W-F814W)
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History:
From electronic version of the journal
License: CC-BY-4.0
(End) Luc Trabelsi [CDS] 19-Jun-2026