PASA 2024

# Dashing through the cluster: An X-ray to radio view of UGC 10420 undergoing
ram-pressure stripping

Smriti Mahajan1 Corresponding author; Email<EMAIL_ADDRESS>Kulinder
Pal Singh1 Juhi Tiwari1 Somak Raychaudhury2,3 1Department of Physical
Sciences, Indian Institute for Science Education and Research Mohali- IISERM,
Knowledge City, Manauli, 140306, Punjab, India  2 Ashoka University, Rajiv
Gandhi Education City, Sonepat, Haryana 131029, India  3 Inter-University
Centre for Astronomy and Astrophysics, Ganeshkhind, Pune, Maharashtra 411007,
India

###### Abstract

We present multi-wavelength data and analysis, including new FUV AstroSat/UVIT
observations of the spiral galaxy UGC 10420 ($z=0.032$), a member of the
cluster Abell 2199. UGC 10420 is present on the edge of the X-ray emitting
region of the cluster at a distance of $\sim 680$ kpc from the centre. The
far-ultraviolet (FUV) data obtained by the AstroSat mission show intense knots
of star formation on the leading edge of the galaxy, accompanied by a tail of
the same on the diametrically opposite side. Our analysis shows that the
images of the galaxy disk in the optical and mid-infrared are much smaller in
size than that in the FUV. While the broadband optical colours of UGC 10420
are typical of a post-starburst galaxy, the star formation rate (SFR) derived
from a UV-to-IR spectral energy distribution is at least a factor of nine
higher than that expected for a star-forming field galaxy of similar mass at
its redshift. A careful removal of the contribution of the diffuse
intracluster gas shows that the significant diffuse X-ray emission associated
with the inter-stellar medium of UGC 10420 has a temperature,
$T_{X}=0.24^{+0.09}_{-0.06}$ keV (0.4–2.0 keV) and luminosity,
$L_{X}=1.8\pm{0.9}\times 10^{40}$ erg s-1, which are typical of the X-ray
emission from late-type spiral galaxies. Two symmetrically placed X-ray hot
spots are observed on either sides of an X-ray weak nucleus.

Our analysis favours a scenario where the interaction of a galaxy with the hot
intra-cluster medium of the cluster, perturbs the gas in the galaxy causing
starburst in the leading edge of the disk. On the other hand, the turbulence
thus developed may also push some of the gas out of the disk. Interactions
between the gas ejected from the galaxy and the intracluster medium can then
locally trigger star formation in the wake of the galaxy experiencing ram-
pressure stripping. Our data however does not rule out the possibility of a
flyby encounter with a neighbouring galaxy, although no relevant candidates
are observed in the vicinity of UGC 10420.

###### doi:

10.1017/pas.2024.xxx

###### keywords:

galaxies: evolution; galaxies: fundamental parameters; galaxies: star
formation; galaxies: individual: UGC 10420

##  1 Introduction

The evolution of galaxies is often accelerated in the vicinity of galaxy
clusters due to the presence of hot intra-cluster medium (ICM), and close
proximity to large neighbouring galaxies. For several decades astronomers have
focused on understanding the various mechanisms responsible for the
morphology-density relation (Dressler, 1980) and star-formation-density
relation (e.g. Balogh et al., 2004) of galaxies. These mechanisms are believed
to be the reason for the presence of more red, elliptical and passively-
evolving galaxies in and near clusters, relative to their counterparts farther
away from the cluster centres.

Gravitational and tidal interactions with comparable-sized neighbours (Toomre
& Toomre, 1972; Moore et al., 1996), emerge as the most important processes
leading to the depletion of gas in galaxies residing in intermediate density
environments such as the cluster outskirts and large-scale filaments (e.g.
Porter & Raychaudhury, 2005; Mahajan et al., 2010, 2012). On the other hand,
ram-pressure stripping (RPS; Gunn & Gott, 1972) plays a significant role in
the evolution of galaxies in the dense interiors of clusters and groups. The
hydrodynamical interaction of the cold gas in a galaxy with the hot ICM can
lead to the evaporation of the interstellar medium (ISM; Cowie & Songaila,
1977), or complete removal of it from the galaxy via RPS. As a consequence,
such a galaxy will eventually cease to form new stars, turn optically red and
become elliptical on timescales of $\sim 1$ Gyr. This idea is in agreement
with the presence of a large number of HI-deficient galaxies in nearby
clusters (e.g. Gavazzi et al., 2006; Haines et al., 2009; Vulcani et al.,
2010; Boselli et al., 2014; Cybulski et al., 2014).

Hydrodynamical simulations, however suggest that in the initial phase, for a
short but significant duration of time RPS can lead to enhancement in the star
formation rate of galaxies (Bekki & Couch, 2003; Bekki, 2014; Steinhauser et
al., 2016; Lee et al., 2020; Troncoso-Iribarren et al., 2020). Using multi-
wavelength datasets, several incidences of starbursts occurring in RPS
galaxies have now been confirmed in nearby clusters (e.g. Crowl et al., 2006;
Yagi et al., 2010; Gavazzi et al., 2015; Vulcani et al., 2018; Boselli et al.,
2022; Lee et al., 2022). In a systematic study of RPS candidates at low-
redshift, Poggianti et al. (2016) found that at fixed mass, these galaxies
have at least twice the rate of star formation relative to unstripped
galaxies.

The environmental processes such as RPS, which influence the gas content of a
galaxy can also impact its nuclear activity. The idea is based on the
observations of enhanced star formation among galaxies experiencing RPS. Due
to the turbulence and instabilities in the disk, resulting from the
interaction of the galaxy with the intra-cluster medium, gas can be funnelled
in towards the galaxy’s centre. This gas can thereby ignite the central
supermassive black hole (Tonnesen & Bryan, 2009), although observational
evidence in favour of these ideas appear debatable at present. In a recent
study of nearby galaxies, a high incidence of optical AGN was found to be
present among RPS galaxies relative to a mass-matched control sample (Peluso
et al., 2022). However, Cattorini et al. (2022) suggest that the results of
Peluso et al. (2022) may be biased by the fact that they are considering both
Seyfert and low-ionization narrow-emission-line region (LINERs) as AGN, and
they are evaluating the AGN fraction with respect to the emission-line
galaxies only. RPS can also have a significant effect on the surface
brightness, temperature and metallicity of the hot interstellar medium of a
galaxy (Kapferer et al., 2009).

In this paper, we present multi-wavelength data and analysis, including new
FUV observations from AstroSat/UVIT for the RPS galaxy UGC 10420 which is a
member of the cluster Abell 2199 ($z=0.031$), and has been observed in many
wavebands from X-ray to radio. Some empirical facts about the X-ray cluster
Abell 2199, sourced from Rines et al. (2016) are provided in Table 2, while
physical properties of UGC 10420 compiled from the literature, or derived for
this analysis, are listed in Table 3. It is noteworthy that UGC 10420 has a
very small radial offset with the cluster’s mean line-of-sight (l.o.s.)
velocity, such that $\Delta v\sim 372$ km s-1. The structure of the paper is
as follows: in the following section we describe various observations and data
used in this paper, followed by our analysis in § 3. In § 4 we discuss the
results in the context of the existing literature, and finally conclude the
paper with an epilogue in § 5. Throughout this work we use concordance
$\Lambda$ cold dark matter cosmological model with $H_{0}=70$ km s-1 Mpc-1,
$\Omega_{\Lambda}=0.7$ and $\Omega_{m}=0.3$ to calculate distances and
magnitudes.

##  2 Observations and data reduction

In this section we describe the source and properties of data compiled for UGC
10420.

###  2.1 Ultraviolet data

UGC 10420 was observed with the ultraviolet imaging telescope (UVIT) aboard
the AstroSat mission (Kumar et al., 2012; Singh et al., 2014; Tandon et al.,
2017). This field (observation ID: A05_063T03_9000003066; PI: Smriti Mahajan;
observation date: 30-July-2019) was observed by the UVIT simultaneously in the
broadband BaF2 FUV filter (mean $\lambda=1541~{}\AA$;
$\Delta\lambda=380~{}\AA$; Tandon et al., 2017, 2020), and visible wavebands
($3040-5500~{}\AA$), although the latter data have not been used for
scientific analysis here. The raw data from the mission are processed by the
Indian Space Science Data Centre (ISSDC), and the Level 1 data from all
instruments are provided to the users. A more comprehensive account of
processing of data and analysis of this field will be presented in an
accompanying paper (Mahajan et al., in preparation), but is briefly mentioned
below for completion.

The UVIT data used in this paper have a total exposure time of 9600.3 seconds
and resolution of $<1.2{{}^{\prime\prime}}$. The L1 data were processed using
the CCDLAB software (Postma & Leahy, 2017), following the procedure described
in Postma & Leahy (2021, also see () for a step-wise account of creating
science images of similar data). The final UVIT FUV image of UGC 10420 is
shown in Fig. 1. For comparison, we show two circles of radii
$0.8{{}^{\prime}}$ and $1.5{{}^{\prime}}$, respectively. While the
$1.5{{}^{\prime}}$ region better captures the UV emission of UGC 10420, the
smaller circle is a better representation of the size of the galaxy at longer
wavebands, as shown below.

Figure 1: This is the AstroSat/UVIT image of UGC 10420. The small red circle
represents the $3{{}^{\prime\prime}}$ diameter SDSS fibre drawn on the optical
centre of the galaxy. The spectrum obtained from this region is shown in Fig.
5, and represents a broadline emission region. The solid blue and dashed black
circles having radius of $0.8^{\prime}~{}\rm{and}~{}1.5^{\prime}$,
respectively are shown for reference to represent the region used for
photometric measurements in various filters. The arrow points in the direction
of the cluster centre.

Figure 2:  (left:) The GALEX  image of UGC 10420 where blue and red represent
the FUV and NUV broadband images, respectively. (right:) This composite image
of UGC 10420 shows the NIR emission in the IRAC 3.6 $\mu$m (blue) and 5.8
$\mu$m (red) bands. A circle of $1.5{{}^{\prime}}$ radius is shown in both the
images for comparison. It is evident that the image of the galaxy is much
smaller in the infrared bands.

UGC 10420 was also observed by the Galaxy and Mass Evolution Explorer (GALEX)
in the near and far ultraviolet broadbands as shown in Fig. 2 (left). It is
noteworthy that the shallow exposure time and poor resolution renders this
image unimpressive relative to the UVIT counterpart shown in Fig. 1. These
data were taken as part of GALEX’s medium imaging survey (MIS), and have a
total exposure time of 1649.1 seconds in both the bands.

In order to measure the flux from UGC 10420, an aperture had to be chosen
manually because the commonly used software split the galaxy into multiple
components due to its large size, and discontinuous emission in almost all
filters. The aperture photometry was performed using the SAOImageDS9 software
package (Joye & Mandel, 2003), by choosing an aperture size of
$1.5{{}^{\prime}}$ centred at the optical nucleus ($\alpha$: 16h29m51.04s;
$\delta$: +39d45m59.42s) for all three UV images. First, we estimated the
background counts by averaging over multiple source-free circular regions of
radius $\geq 1.5{{}^{\prime}}$, and subtracted them from the counts obtained
for the region centred on UGC 10420. The counts were then converted to fluxes
using the standard conversion factors given in Tandon et al. (2020) for the
UVIT image, and
https://asd.gsfc.nasa.gov/archive/galex/FAQ/counts_background.html for the
GALEX  images, respectively. The final flux values, measurement uncertainty in
flux, and the effective wavelength for all wavebands are listed in Table 1.

Figure 3: (left:) The combined $B,R$ and $I$ band digitized sky survey (DSS) image of the sky around UGC 10420. The central elliptical galaxy of Abell 2199, NGC 6166 is marked along with the X-ray centre of the cluster (red cross; Mahdavi & Geller, 2001) at the bottom right to show the relative position of UGC 10420 in the cluster. (right:) This is an optical $g,r,i$ image of UGC 10420 created using the SDSS photometric data. North is up and east is on the left for both images. Table 1: Integrated flux measurements for UGC 10420 in different wavebands, in increasing order of wavelength from top to bottom.  Filter | Effective $\lambda$ | Flux | Uncertainty in flux | Source
---|---|---|---|---
| (Å ) | (mJy) | (mJy) |
GALEX $FUV$ | 0.152 | 1.486 | 4.00E-01 | measured from image
UVIT BaF2 | 0.154 | 2.030 | 8.04E-03 | measured from image
GALEX $NUV$ | 0.232 | 2.315 | 2.90E-01 | measured from image
SDSS $u$ | 0.356 | 2.573 | 9.66E-02 | measured from image
$U$ | 0.357 | 3.060 | 2.64E-00 | from Gil de Paz et al. (2007)
$B$ | 0.446 | 6.877 | 5.99E-00 | from Gil de Paz et al. (2007)
SDSS $g$ | 0.477 | 6.920 | 1.58E-01 | measured from image
$V$ | 0.550 | 11.197 | 9.66E-00 | from Gil de Paz et al. (2007)
SDSS $r$ | 0.623 | 11.410 | 2.03E-01 | measured from image
SDSS $i$ | 0.763 | 15.438 | 2.37E-01 | measured from image
SDSS $z$ | 0.913 | 18.375 | 2.58E-01 | measured from image
$J$ | 1.200 | 18.370 | 17.87E-00 | from Gil de Paz et al. (2007)
$H$ | 1.620 | 19.653 | 18.77E-00 | from Gil de Paz et al. (2007)
$K$ | 2.200 | 12.767 | 11.86E-00 | from Gil de Paz et al. (2007)
WISE $W1$ | 3.368 | 12.922 | 2.84E-02 | measured from image
IRAC $I1$ | 3.560 | 14.254 | 3.76E-01 | measured from image
WISE $W2$ | 4.618 | 7.653 | 2.14E-02 | measured from image
IRAC $I3$ | 5.760 | 14.457 | 9.95E-01 | measured from image
WISE $W3$ | 12.082 | 13.993 | 0.17E-00 | measured from image
WISE $W4$ | 22.194 | 16.027 | 0.75E-00 | measured from image
Radio 144 MHz | 2.087E+10 | 74.670 | 0.17E-00 | measured from image

###  2.2 X-ray Data

UGC 10420 was in the field of view of an observation with the XMM-Newton
EPIC111The European Photon Imaging Camera onboard the XMM-Newton observatory..
This observation (Obs. ID: 0784521201, PI: Takayuki Tamura, Obs. time: 40 ks)
carried out on 2017 March 17 was centred at $\alpha$: 16h30m32s and $\delta$:
+39d44m52s and focused on the intermediate regions ($<3/4$ virial radius) of
Abell 2199. All the three detectors aboard XMM-Newton, viz., EPIC PN, MOS1 amd
MOS2 detectors were operated in the Full Frame mode and medium optical
blocking filter was used. The dataset for this observation was retrieved from
the HEASARC222High Energy Astrophysics Science Archive Research Center;
https://heasarc.gsfc.nasa.gov/ archive, then processed and analysed using the
XMM-Newton Science Analysis System (SAS) version 20.0.0 and the Extended
Source Analysis Software (XMM-ESAS) package integrated into SAS. The latest
calibration files were employed to produce the PN (MOS) event files using the
SAS tasks epchain (emchain).

The X-ray data were first screened to remove the particle backgrounds as
described below:

a) The event files were filtered for soft proton (SP) background flares using
the tasks pn-filter and mos-filter. The SP flare filtering resulted in useful
exposure times of 28.92, 35.46, and 38.20 ks for the PN, MOS1, and MOS2
detectors, respectively. We examined the output of the task mos-filter and
verified that none of the MOS detectors operated in an anomalous state during
the observation.
b) The events arising due to quiescent particle background (QPB) produced by
the interaction of high energy particles ($>100$ MeV) with the X-ray detectors
and the surrounding structure was then removed. QPB shows only small intensity
variations over the time scale of a typical X-ray observation, and therefore
not detected as flares. The standard norm to subtract out the QPB contribution
from the data is to either use blanksky observations or model the QPB. The
XMM-ESAS package models the QPB using a combination of a database of
unexposed-region data and filter-wheel-closed data based on the methods of
Kuntz & Snowden (2008), and we have used this method to model and subtract the
QPB instead of using blanksky files.

The filtered event files thus produced were used for making the images and
spectra, and analysed as described below.

The XMM-ESAS tasks pn-spectra (mos-spectra) followed by pn$\\_$back
(mos$\\_$back) were used to generate the PN (MOS1/MOS2) images of UGC 10420 in
three different energy bands (one at a time), viz. soft: $400-2000$ eV, hard:
$2000-7000$ eV, and total: $400-7000$ eV, by setting the elow and ehigh energy
parameters to the requisite values (unit: eV). These tasks also generated the
QPB images and exposure maps for each EPIC detector. The individual PN, MOS1,
and MOS2 counts images, exposure maps, and model QPB images were then combined
into a single counts, exposure, and QPB image using the task comb. Finally, a
combined PN, MOS1, and MOS2 particle-background-subtracted, exposure-
corrected, and adaptively smoothed surface brightness image of UGC 10420 was
generated using the task adapt. A smoothing scale of 10 counts and a pixel
size of $2.5{{}^{\prime\prime}}$ were used. X-ray images of UGC 10420 in the
three energy bands are shown in Figure 4. The nuclear region around the
optical centre appears to be very faint and soft in X-rays, with two bright
spots, neither of which is coincident with the optical centre, and surrounded
by some diffuse emission. Emission from the central region cannot be seen in
the hard X-ray band, however. The two bright sources far away from the nuclear
region on the east and west are confirmed as point sources using the ESAS task
cheese, which runs point source detection by calling the SAS task
edetect$\\_$chain. We used a detection box of $5\times 5$ pixels for this
purpose. Further analysis of these X-ray sources is presented in §3.3.

Figure 4: left to right: Particle-background-subtracted, exposure-corrected, combined PN, MOS1, and MOS2 XMM-Newton surface brightness image of UGC 10420 in the soft (0.4–2.0 keV), hard (2.0–7.0 keV), and total (0.4–7.0 keV) X-ray energy bands. The surface brightness contours are as follows – soft band: 6 levels (9.9, 20.9, 36.1, 61.1, 105.0, and 184.3 cts s-1 deg-2) between 3$\sigma$ and $88\sigma$ above a background level of 3.7 cts s-1 deg-2; hard band: 3 levels (17.1, 30.8, and 81.3 cts s-1 deg-2) between 3$\sigma$ and 19$\sigma$ above a background level of 5.1 cts s-1 deg-2; total band: 5 levels (16.5, 43.9, 87.4, 172.8, and 350.2 cts s-1 deg-2) between $3\sigma$ and $98\sigma$ above a background level of 6 cts s-1 deg-2. In each panel, the $\times$ symbol marks the optical centre of UGC 10420, and the $+$ symbols mark the centres of the two X-ray point sources detected in the galaxy. The solid white and dashed white circles represent the $1.5{{}^{\prime}}$ and $0.8{{}^{\prime}}$ radius apertures, respectively, centred at the optical centre. Table 2: Empirical facts about Abell 2199 (Rines et al., 2016).  Parameter | Value
---|---
Right Ascension (J2000) | 16 28 37.90
Declination (J2000) | +39 32 55.32
Redshift ($z$) | 0.0309
Velocity dispersion ($\sigma$) |  $676^{+37}_{-32}$ km s-1
$M_{200}$ |  $(2.39\pm 0.77)\times 10^{14}$ M⊙
Table 3: Observed properties of UGC 10420, a member galaxy of cluster Abell 2199.  Parameter | Value | Reference
---|---|---
Right Ascension (J2000) | 16 29 51.04 | SDSS database
Declination (J2000) | +39 45 59.42 | SDSS database
Redshift ($z$) | 0.03185 | SDSS database
Luminosity distance ($D_{L}$) | 139.7 $h^{-1}$ Mpc | -
Scale (kpc/′′) | 0.636 | -
Morphological type | SB(c) | Buta (2019)
Position angle (PA) of stellar bar | $89.9^{\circ}$ | Fraser-McKelvie et al. (2020)
Length of stellar bar | 3.9 kpc | Fraser-McKelvie et al. (2020)
Petrosian 50% radius in $r$-band, $R_{50,r}$ | $18.2{{}^{\prime\prime}}$ | Fraser-McKelvie et al. (2020)
Milkyway extinction, $E(B-V)$ | 0.0085 | Schlafly & Finkbeiner (2011)

###  2.3 Optical data

The optical photometric and spectroscopic data used in this paper are sourced
from the Sloan Digital Sky Survey (SDSS, data release 14; Abolfathi et al.,
2018), unless mentioned otherwise. The SDSS images have an exposure time of
53.9 seconds in each of the five filters $u,g,r,i,z$. Photometry was performed
in all five wavebands using an aperture size of $0.8{{}^{\prime}}$, following
the procedure described in Sec. 2.1. The measured counts were then converted
to fluxes using the standard conversion factor from maggies to Jy, and are
listed in Table 1.

In Fig. 3 (left), we show the position of the galaxy relative to the centre of
Abell 2199, on the digitized sky survey (DSS) image of the field. UGC 10420 is
$\sim 680$ kpc away from the cD galaxy NGC 6166 of the cluster. A composite
$g,r,i$ image of UGC 10420, shown in Fig. 3 (right), clearly shows the
asymmetry in the spiral arms of UGC 10420, and the presence of a bar at the
centre, in agreement with the morphological classification of type SB(c)
(Buta, 2019). Even though the outer regions of UGC 10420 are optically blue,
majority of the optical emission from the disk is dominated by red stellar
populations, as quantified by a colour value of $(g-r)\sim 0.8$ mag, which is
typical for passively-evolving late-type galaxies (e.g. Mahajan &
Raychaudhury, 2009; Song et al., 2017; Mahajan et al., 2020).

The optical spectrum of UGC 10420 obtained from the $3{{}^{\prime\prime}}$
diameter SDSS fibre is shown in Fig. 5 (also see Fig. 1 for a comparison
between the size of the fibre relative to the galaxy). On the basis of
emission line fluxes obtained from this spectrum, UGC 10420 is classified as a
LINER galaxy, using the BPT (Baldwin et al., 1981) emission-line diagnostic
diagram (Toba et al., 2014).

Figure 5: The spectrum (black line) from the nuclear region of UGC 10420 (also
see Fig. 1), based on which it is classified as a LINER galaxy. The blue and
grey lines represent the best-fit model to the spectrum, and emission from the
sky, respectively. The model spectrum is offset along the ordinate for
clarity, and the corresponding shifted axis is shown in blue on the right. All
the data shown in this image are sourced from the SDSS database.

###  2.4 Infrared data

The infrared (IR) observations for UGC 10420 were obtained from the Infrared
Science Archive (IRSA) of the NASA Infrared Processing and Analysis Center
(IPAC)333https://irsa.ipac.caltech.edu/about.html. For this work we used the
images from the Wide-field Infrared Survey Explorer (WISE; Wright et al.,
2010), as well as the Infrared Array Camera (IRAC) aboard the Spitzer mission.

WISE observed the sky in the near- and mid-infrared wavebands between 3.6 to
22 $\mu$m. We performed photometry on all the four band ALLWISE images, and
channels 1 and 3 IRAC images (3.6 and 5.8 $\mu$m, respectively) in the same
manner as described in sec. 2.1, but using an aperture of $0.8{{}^{\prime}}$.
Our choice of aperture size is dictated by the fact that the UGC 10420’s image
is much smaller in these bands, and, the aperture of $1.5{{}^{\prime}}$ used
for the UV data would include many galactic and extragalactic sources not
visible in other bands, thereby contaminating the flux measurement. The
estimated fluxes are listed in Table 1. A glimpse of the IR emission relative
to the light in the optical and FUV filters can be seen in Fig. 2 (right) and
Fig. 6. Figs. 1–3 and 5 show that the optical-IR emission is concentrated in
the central region of the galaxy encompassing the nucleus and the stellar bar,
where as the FUV emission dominates the outer regions of the galaxy.

Figure 6: A composite image of UGC 10420 created using the IRAC 3.6 $\mu$m
(red), SDSS $g$-band (green) and UVIT FUV (blue) data, respectively. Despite
different pixel sizes and depth of the three datasets, this image shows the
distorted spiral arms of UGC 10420which are likely perturbed by the
interaction with the intra-cluster medium. It is also evident that most of the
star-formation is now occurring in the outer regions of the galaxy.

###  2.5 Radio data

The radio image of UGC 10420 is obtained from the data release 2 of the
ongoing LOw-Frequency ARray (LOFAR) Two-metre Sky Survey (LoTSS; 120–168 MHz;
Shimwell et al., 2022). The LoTSS images were derived from the LOFAR high band
antenna data, which were corrected for the direction-independent instrumental
properties as well as direction-dependent ionospheric distortions with fully
automated, data processing. At $\sim 6{{}^{\prime\prime}}$ resolution, the
full bandwidth Stokes I continuum maps of these data at a central frequency of
144 MHz, have a median root mean square (rms) sensitivity of
$83~{}\mu$Jy/beam, a flux density scale accuracy of approximately 10%, and
astrometric accuracy of $0.2{{}^{\prime\prime}}$.

The radio flux density mentioned in Table 1 was obtained using aips. In order
to determine the flux density, the counts in a polygon region centred at UGC
10420 were determined and divided by the area covered by the beam. The
uncertainty in the flux was calculated as the product of the square root of
the number of beams within the polygon region, and the rms uncertainty
($=0.017$ mJy) in a similar sized source-free region. The flux density scale
uncertainty for the LoTSS data is found to be $\sim 6\%$ (Shimwell et al.,
2022). The 144 MHz emission encompasses the optical disk of the galaxy as
shown in an optical-UV-radio composite image of UGC 10420 in Fig. 7. The radio
emission appears to be orientated along the direction of motion of the galaxy
with a gap in the middle, in line with the FUV image of the galaxy (Fig. 1).

Figure 7: This composite image of the UGC 10420 shows the low-frequency LOFAR
radio emission (red), the optical $g$-band (green) and the UVIT FUV emission
(blue), respectively. The synthesised radio beam is represented by the
$6{{}^{\prime\prime}}$ radius circle at the bottom right. It is noteworthy
that an excess of radio emission is detected in the northwestern part of the
galaxy, opposite to the direction of the cluster centre. The arrow points in
the direction of the cluster centre.

##  3 Analysis and Results

###  3.1 Spectral energy distribution

Figure 8: The integrated UV to near-infrared spectral energy distribution
(SED) of the galaxy UGC 10420. In the top panel, photometric data from Table 8
are shown as black points. These data are used to fit an SED using the code
magphys (da Cunha et al., 2008). The attenuated (red line), and unattenuated
(blue line) best-fit SEDs are also shown. The residuals with respect to the
best-fit are shown in the bottom panel. Also see Table 4 for the physical
parameters derived from this SED.

The arsenal of data mentioned in Section 2 can be used to derive useful
information about the stars, gas and dust of UGC 10420 by means of its
spectral energy distribution (SED). In this work we use the self-contained
model package called Multi-wavelength Analysis of Galaxy Physical Properties
(magphys; da Cunha et al., 2008) to model the SED of UGC 10420. magphys takes
the photometric data from UV to IR wavebands as input, to model the attenuated
and unattenuated SED of a galaxy. It makes use of the stellar evolution models
by Bruzual & Charlot (2003), assuming a Chabrier (2003) initial mass function
and a Charlot & Fall (2000) attenuation law. For UGC 10420 we input the data
listed in Table 1 (sans radio flux).

The output is shown in Fig. 8, and some of the derived physical parameters:
star formation rate (SFR)444Since this SFR is based on Chabrier (2003) IMF, we
have divided by 0.63 (Madau & Dickinson, 2014) to convert to the Salpeter IMF
used throughout this work., stellar mass ($M^{*}$), dust mass (MDust) and
specific star formation rate (SFR/$M^{*}$; sSFR henceforth) are listed in
Table 4, respectively. The physical properties of UGC 10420 are typical of
optically-selected red spiral galaxies explored in the literature (e.g.
Mahajan et al., 2020).

Table 4: Some physical parameters estimated from the SED of UGC 10420 fitted using the magphys code (da Cunha et al., 2008).  Parameter | Value
---|---
SFR, $M_{\odot}$ yr-1 | $9.75$
Stellar mass, $M^{*}/M_{\odot}$ | $1.8\times 10^{10}$
Dust mass, $M_{Dust}/M_{\odot}$ | $6.8\times 10^{6}$
SFR/$M^{*}$ | $3.4\times 10^{-10}$

###  3.2 Star forming regions

Figure 9: (a) Individual ‘regions’ detected by the sextractor overlaid on the
UVIT image are shown. The regions are colour-coded as follows: the regions
with little to no optical emission are classified as XUV regions shown in
(blue), those which have optical emission in the $g$-band, and lie
$>0.5^{\prime}$ away from the optical centre as regions in galaxy (solid
black), respectively. Objects marked as B1 and B2 are background galaxies and
not considered in our analysis. The counterparts of the latter form the bulk
of the galaxy photometry in almost all the filters (and hence are very
different from the smaller star-forming regions/clumps explored in this
analysis) are shown as (dashed black) circles. The other panels show a
comparison between the (b) SFR determined from FUV luminosity, (c) the FUV-NUV
colour, and (d) surface brightness of the regions in the galaxy (solid black),
and the XUV regions (hatched blue), respectively. It is evident that the XUV
regions are bluer, brighter and have lower SFR relative to similar regions
closer to the centre of the galaxy.

It has been shown that the detection of extended UV (XUV) emission beyond the
optical extent of the galaxy is not very uncommon in nearby star-forming
galaxies (e.g. Thilker et al., 2007). A comparison between this star formation
far away from the centre of the galaxy, and that in the optical disk is
therefore crucial in understanding star formation processes. Moreover, we are
unaware of any XUV disk observed in clusters, which makes UGC 10420 a very
unique galaxy.

We take advantage of the high resolution of the UVIT to get a better
perspective on the individual regions which have been resolved in UGC 10420.
In order to do so, we classified these regions based on their distance from
the centre of the galaxy. As shown in Fig. 9(a), all regions $>0.5^{\prime}$
from the centre of the galaxy are classified as XUV regions (blue circles),
and are mostly located outside the optical disk of the galaxy. Most of these
XUV regions have a faint or no optical counterpart in the SDSS $g$-band image.
The regions which are part of the galactic disk are further sub-classified
into two categories: regions which are comparable to the XUV regions in size
and luminosity, and having an optical counterpart are shown in solid black
circles; these are henceforth referred to as the inner regions. Secondly, the
regions closer to the centre of the galaxy, which form the bulk of the
emission from UGC 10420 in almost all filters are represented by dashed black
circles. In total there are 21 XUV regions which are compared to 13 inner
regions, while the 11 innermost regions are ignored in the following analysis
because they are much more luminous (and massive) than the XUV regions. The
objects marked as B1 and B2 are background galaxies, and are ignored
hereafter.

FUV light is emitted by stars with masses of several solar masses, and a mean
age of 10 Myr ($10-100$ Myr), with the shortest wavelengths corresponding to
the shortest timescales (Hao et al., 2011; Murphy et al., 2011; Kennicutt &
Evans, 2012). The UV continuum emission from 1200 to 3200 Å is therefore an
inevitable consequence of recent star formation. As a result, FUV luminosity
is a direct tracer of recent star formation (few tens of Myr) occurring in a
galaxy, and can be used to estimate the rate of star formation (SFR). In this
work we employ the prescription provided by Iglesias-Páramo et al. (2006):

${\rm log(SFR}_{FUV}/{\rm M}_{\odot}~{}yr^{-1})={\rm
log}(L_{FUV}/L_{\odot})-9.51$ (1)

where, $L_{FUV}$ is the FUV luminosity of the galaxy corrected for galactic
extinction ($A_{FUV}$). The calibration for this prescription is derived from
Starburst99 models (Leitherer et al., 1999), assuming a solar metallicity and
a Salpeter IMF from $0.1-100~{}{\rm M}_{\odot}$. Galactic extinction,
$A_{FUV}=8.06\times E(B-V)$ (Bianchi, 2011), where the colour excess
$E(B-V)=0.0085$ for UGC 10420 is obtained from the dust reddening maps of
Schlafly & Finkbeiner
(2011)555https://irsa.ipac.caltech.edu/applications/DUST/.

Fig. 9(b) shows a comparison between the SFR estimated for the XUV regions,
and the inner regions using the SFR derived from UVIT data. It is notable that
the XUV regions on average have lower SFR and smaller dispersion relative to
similar regions closer to the centre of the galaxy. Specifically, the mean and
standard deviation of SFR for the XUV regions is $0.014\pm 0.008~{}{\rm
M}_{\odot}~{}yr^{-1}$, relative to the value for the inner regions $0.035\pm
0.028~{}{\rm M}_{\odot}~{}yr^{-1}$. The Kolmogorov-Smirnov (KS) statistical
test probability ($p$), in favour of the hypothesis that the two distributions
are drawn from the same parent sample is 1.77E-03, thus suggesting that they
are disparate. Furthermore, the XUV regions have bluer $FUV-NUV$ colours (Fig.
9(c); $p=$ 2.99E-02), and are brighter than the inner regions (Fig. 9(d); $p=$
2.09E-03). The respective mean surface brightness value for the XUV regions is
$42.8\pm 12.1$ magnitude arcseconds-2, relative to only $26.1\pm 7.2$
magnitude arcseconds-2 for the inner regions.

It is noteworthy that even though a correction for internal extinction is
important when converting FUV luminosity to SFR (e.g. Mahajan et al., 2019),
in this case we are unable to do so because of the unavailability of FIR data,
and hence the estimated SFRs may be regarded as lower limits. The result from
these comparisons therefore should only be considered in a qualitative sense,
assuming that the internal extinction in the XUV regions and inner regions is
the same. Also, resolution effects may play a significant role in this
comparison, since only the most massive star-forming regions may be resolved
at the distance of UGC 10420. Most of the ‘regions’ considered here, therefore
may be much larger than typical star-forming regions observed in nearby
galaxies.

This distinction suggests that the XUV regions are statistically different
from the inner regions. In our opinion, these qualitative differences suggest
that they have different origins. As UGC 10420 interacts with the surrounding
ICM, some of the cold atomic gas from the galaxy is stripped, leaving a wake
in the direction opposite to the direction of the motion of the galaxy. The
fact that the cluster centre lies diametrically opposite to the direction of
the XUV tail(s) pointing towards the north-east, forms the basis of this idea.
Star-forming regions beyond the optical disk have been observed in several
other nearby galaxies (e.g. Cortese et al., 2007; Werk et al., 2010; Poggianti
et al., 2017; Boselli et al., 2021). In particular, the galaxy IC 3476 in the
Virgo cluster which is experiencing edge-on stripping is worth mentioning,
since it shows HII regions in the two diametrically opposite ends of the
galaxy just like UGC 10420 (see fig. 4 of Boselli et al., 2021). Also, even
though we only have access to the low-frequency radio data for UGC 10420, it
is evident from Fig. 7, that there is more radio emission on the trailing edge
of the galaxy relative to the western side facing the cluster centre. In this
situation, the inner regions are formed where the stripped gas experiences a
shock, while the XUV regions are formed in the wake of the RPS gas tails.

Figure 10: X-ray image in the energy band 0.4–2.0 keV showing the location of
UGC 10420 within its host galaxy cluster Abell 2199. The galaxy is located at
a projected distance of $\sim 680$ kpc from the X-ray peak of Abell 2199. The
small red circle (labelled UGC 10420) is used for estimating the properties of
the diffuse X-ray emission associated with UGC 10420. The partial annular
regions sandwiching UGC 10420 (highlighted in red colour and labelled A2199
ICM) are used for estimating the properties of the Abell 2199 ICM at the
location of the galaxy.

###  3.3 Diffuse X-ray emission from UGC 10420

In §2.2 we pointed out the existence of diffuse soft X-ray emission connecting
two bright point-like sources and the nucleus of the galaxy (Fig. 4 left
panel). Here, we have tried to isolate the diffuse component in UGC 10420 and
study its properties. The properties of the point sources are studied and
presented in the next section. In Figure 10, we show the X-ray emission from
Abell 2199 and its outskirts. The location of UGC 10420 with respect to Abell
2199 is also shown. This figure was derived from both the current observation
and another XMM-Newton observation centered on the cluster centre. To isolate
and study the properties of the diffuse X-ray emission associated with the
galaxy, we have to estimate and remove the contribution of the backgrounds,
cluster emission and the point sources.

We performed spectral analysis of emission within the red circular region
(radius: $1.5{{}^{\prime}}$; label: UGC 10420) shown in Figure 10 to estimate
the properties of overall diffuse X-ray emission from UGC 10420. The
contribution from the two point sources in UGC 10420, shown in Figure 4, was
removed using the mask image generated by the task cheese (Sec. 2.2). The
source spectrum, the modelled background spectrum, and the spectral response
of the EPIC were extracted within the red circular region encompassing the
diffuse emission in UGC 10420 using the tasks pn-spectra (mos-spectra) and
pn$\\_$back (mos$\\_$back). All spectra were suitably grouped using the FTOOL
grppha (HEASoft version 6.30.1), and analysed using XSPEC version 12.12.1
(Arnaud, 1996). The diffuse background components towards UGC 10420 include
the diffuse soft X-background (SXRB) and the cosmic X-ray background (CXB)
which are described in detail in Tiwari & Singh (2021). Since UGC 10420 is
located in the outskirts of Abell 2199, there is also a significant
contribution from the intracluster gas. Therefore, in addition to the X-ray
background components, it is also necessary to account for the emission from
the ICM of Abell 2199 at the galaxy’s location, when modelling its diffuse
emission, as described below.

The partial annular regions sandwiching UGC 10420 shown in Figure 10 (label:
A2199 ICM) were used to estimate the properties of the intracluster gas in the
region around the galaxy. The PN, MOS1, and MOS2 spectra extracted from these
annular regions were fitted jointly in the energy range 0.4–7.0 keV with the
Rosat All Sky Survey (RASS) diffuse background spectrum using the model
constant*(apec+tbabs*(apec+apec+pegpwrlw) + tbabs*apec). We refer the reader
to Tiwari & Singh (2021) for definitions of the individual XSPEC models and
details of the background modeling. For completeness, we mention that the
model component apec+tbabs*(apec+apec+pegpwrlw) in the expression above
represents the complete X-ray background (SXRB + CXB). The second model
component tbabs*apec represents the absorbed X-ray emission from the cluster
outskirts. The constant factor is used to scale the model normalization of the
PN, MOS1, and MOS2 data to ensure consistency with the RASS spectral data
which is in units of cts s-1 arcmin-2. We fixed the total Hydrogen column
density, $N_{H}$, along the line of sight to UGC 10420/Abell 2199 outskirts to
$9.63\times 10^{19}$ cm-2, based on the work of Willingale et al.
(2013)666https://www.swift.ac.uk/analysis/nhtot/. The redshift was frozen at
0.03185. Two additional models – gauss (1.49 keV) and gauss (1.75 keV) – were
used to model the instrumental background lines – the Al K$\alpha$ line at
$\sim$1.49 keV for PN, MOS1, and MOS2, and the Si K$\alpha$ line at $\sim$1.75
keV for the MOS1 and MOS2 detectors – as and when required.

The intracluster gas at the location of UGC 10420 was found to have a
temperature of $3.3^{+0.9}_{-0.7}$ keV and metallicity of $\sim$0.2 Z⊙
($\chi^{2}=366.07$, $\text{dof}=354$). These properties of the ICM of Abell
2199 are in agreement with previous studies by Kawaharada et al. (2010) and
Mirakhor & Walker (2020).

The properties of the diffuse X-ray emission associated with UGC 10420 were
then estimated by fitting the PN, MOS1, and MOS2 spectra extracted from the
red circular region in Figure 10 simultaneously with the RASS background data
using the model constant*(apec+tbabs*(apec+apec+pegpwrlw) +
tbabs*(apec+apec)). The newly added apec component represents emission from
the hot interstellar gas in the galaxy. The other model components have the
same definitions as described previously. Here, the spectral parameters for
the X-ray background, and the temperature and abundance of the Abell 2199 ICM
were fixed based on the results of the spectral analysis mentioned above. The
energy range 0.4–7.0 keV was used for the spectral fitting. We found the hot
gas in UGC 10420 to have a temperature of $0.24^{+0.09}_{-0.06}$ keV, with the
metal abundance, Z, frozen at the solar value ($\chi^{2}=104.53$, dof$=114$).
If the abundance was left free to vary during the fit, we obtained Z $=0.8$ Z⊙
with the gas temperature unchanged, but the errors in the abundance could not
be constrained due to low number of counts.

###  3.4 X-ray emission from the two hot spots and nuclear region

Figure 11: The total band (0.4–7.0 keV) X-ray image showing the eastern and
western X-ray point sources in UGC 10420. The ${\bf\times}$ symbol marks the
optical centre of UGC 10420. The solid white circles mark the regions used for
the spectral extraction and analysis of each point source.

Spectral analysis of the two bright point sources in UGC 10420 was carried out
by extracting spectra from the circular regions shown in Figure 11 to estimate
their general properties. These relatively large regions, extending beyond the
actual size of the detected sources, were used so as to enclose enough counts
to make the spectral modelling possible. Since these circular regions also
enclose the diffuse emission from the cluster and galaxy, we accounted for
these contributions in the spectral analysis as described above. The spectrum
of each point source was well fitted by a power-law777The power-law photon
spectrum has the form $KE^{-\alpha}$, where $\alpha$ (dimensionless) is the
photon index of the power-law, and $K$ is the normalization in units of
photons keV-1 cm-2 s-1 at 1 keV. in the energy range 0.4–7.0 keV. The
unabsorbed flux (luminosity) of each point source was estimated by convolving
the powerlaw model with the XSPEC model cflux (clumin) after freezing the
power-law model normalization. The results of the spectral analysis and the
derived properties of the two point sources are given in Table 5.

Table 5: Properties of the two X-ray point sources in UGC 10420. The errors in photon index, flux, and luminosity are quoted at 90 per cent confidence level. | R.A. (J2000) | Dec. (J2000) | Photon index ($\alpha$) |  $\chi^{2}$ (dof) | Flux | Luminosity
---|---|---|---|---|---|---
|  |  |  |  | (0.4–7.0 keV) | (0.4–7.0 keV)
|  |  |  |  | erg cm-2 s-1 | erg s-1
Eastern source | 16h29m53.92s | +39d46m01.67s | $1.8^{+0.3}_{-0.2}$ | 20.45 (34) | $2.6\pm{0.4}\times 10^{-14}$ | $6.7\pm{1.1}\times 10^{40}$
Western source | 16h29m47.41s | +39d45m31.78s | $1.6\pm{0.2}$ | 61.13 (58) | $4.9\pm{0.5}\times 10^{-14}$ | $1.2\pm{0.1}\times 10^{41}$

The unabsorbed X-ray flux and luminosity of the entire galaxy (hot spots +
diffuse emission) were estimated within two circular apertures of radii
$0.8{{}^{\prime}}$ and $1.5{{}^{\prime}}$ centred at the optical centre of the
galaxy (see Figure 4). In order to do so, the PN, MOS1, and MOS2 spectra
extracted within the $1.5{{}^{\prime}}$ radius aperture were simultaneously
fitted with the RASS data using the model
constant*(apec+tbabs*(apec+apec+pegpwrlw) + tbabs*(apec+ apec + powerlaw +
powerlaw)). The highlighted model component represents the total X-ray
emission – point sources + diffuse – from UGC 10420. Here, apec represents the
diffuse emission from UGC 10420, and the two powerlaw components model the
emission from the two point sources in UGC 10420 which lie within the aperture
of radius $1.5{{}^{\prime}}$. For modelling the X-ray spectrum within the
smaller aperture of radius $0.8{{}^{\prime}}$, we used only one powerlaw model
since only the eastern point source falls within this aperture. The X-ray flux
in the two apertures was then estimated by convolving the apec + powerlaw +
powerlaw component with the XSPEC model cflux. Similarly, the total X-ray
luminosity was estimated using the XSPEC convolution model clumin. The total
X-ray flux and luminosity values for the two apertures in the soft, hard, and
total bands are reported in Table 6.

A limit to the soft X-ray flux from the nuclear region, which is not fully
resolved, was estimated from the PN data in the soft band and using a circular
region with a radius of 9 arcsec. Scaling the estimated PN background to the
same size, we obtain a 3$\sigma$ upper limit on the soft emission from the
nuclear region around the optical centre to be $\sim$0.004 counts s-1.
Assuming the central source to have a photon index of 2, this limit translates
to a flux of 5.4$10^{-15}$ erg cm-2 s-1 in the soft energy band, giving a
3$\sigma$ limit on luminosity of 1.4 $10^{40}$ ergs s-1 for an AGN like source
in the centre.

Table 6: Total unabsorbed X-ray flux ($F_{X}$ in erg cm-2 s-1) and luminosity ($L_{X}$ in erg s-1) estimates of UGC 10420. The errors are quoted at 90 per cent confidence level.  Aperture radius | Soft band | Hard band | Total band
---|---|---|---
| (0.4–2.0 keV) | (2.0–7.0 keV) | (0.4–7.0 keV)
$1.5{{}^{\prime}}$ |  $F_{X}$: $3.7\pm{0.5}\times 10^{-14}$ |  $F_{X}$: $3.6^{+0.4}_{-0.5}\times 10^{-14}$ |  $F_{X}$: $7.3\pm{0.9}\times 10^{-14}$
|  $L_{X}$: $9.3\pm{1.1}\times 10^{40}$ |  $L_{X}$: $9.1\pm{0.9}\times 10^{40}$ |  $L_{X}$: $1.8\pm{0.2}\times 10^{41}$
$0.8{{}^{\prime}}$ |  $F_{X}$: $2.5\pm{0.3}\times 10^{-14}$ |  $F_{X}$: $2.2\pm{0.3}\times 10^{-14}$ |  $F_{X}$: $4.7\pm{0.6}\times 10^{-14}$
|  $L_{X}$: $6.2\pm{0.7}\times 10^{40}$ |  $L_{X}$: $5.7^{+0.6}_{-0.8}\times 10^{40}$ |  $L_{X}$: $1.2\pm{0.1}\times 10^{41}$

##  4 Discussion

In this paper we have presented the UVIT FUV data and ancillary data in other
wavebands for the spiral galaxy UGC 10420, a member of the cluster Abell 2199.
Our analysis shows that this galaxy, at a projected distance of $\sim 680$ kpc
from the cluster’s centre is being ram-pressure stripped by the ICM of the
cluster. It is notable that the l.o.s. velocity offset of UGC 10420 with
respect to the mean velocity of Abell 2199 is only $\sim 372$ km s-1, which is
much smaller than the velocity dispersion of the cluster. This, together with
the FUV observations presented in this work, suggests that UGC 10420 must be
moving with a very high speed towards the cluster centre, in a direction
normal to the l.o.s.. As a consequence of stripping, the outer spiral arms of
the galaxy are being removed and turned into what looks like a wake of star-
forming knots on the south-eastern side of the galaxy (Fig. 1). These
observations agree with the simulations of RPS galaxies suggesting that the
SFR increases in the gaseous wake of the galaxy rather than the disk itself,
and hence is strongly dependant on the density of the surrounding ICM
(Kapferer et al., 2009).

There is an increasing consensus building up in the recent literature that
most of the enhanced star formation in RPS galaxies is observed on the
‘leading edge’ of the galaxies (Gavazzi et al., 2015; Vulcani et al., 2018;
Hess et al., 2022; Roberts et al., 2022a). Such galaxies, showing an
unambiguous tail of material stripped from the disk are often called the
‘jellyfish galaxies’, and are considered to be a product of RPS in clusters.
It is believed that the stripped gas must cross the entire galaxy disk before
leaving it, and therefore is more likely to cause instabilities and
turbulence, which in turn triggers starburst in jellyfish galaxies (Boselli et
al., 2022). Several examples of such jellyfish galaxies have been
observationally discovered (Poggianti et al., 2016; Vulcani et al., 2018;
Safarzadeh & Loeb, 2019; Lee et al., 2020; Cramer et al., 2021; Roberts et
al., 2022b). The FUV observations of UGC 10420, showing intense star-forming
knots on the western side of the disk (Fig. 1), also favours this scenario.

In order to test the significance of the increase in the SFR of UGC 10420, we
adopted the following SFR main sequence relation derived by Speagle et al.
(2014) as a function of stellar mass and cosmic time:
${\rm log~{}SFR}(M^{*},t)=(0.84-0.026t){\rm log}M^{*}-(6.51-0.11t)$,
where, $t$ is the age of the Universe (Gyr) at the redshift of the galaxy. In
line with many other observations in the literature (Lee et al., 2022, and
references therein), we find that the SED derived SFR of UGC 10420 is at least
a factor of nine larger than that expected for star-forming field galaxies of
similar mass at $z\sim 0.03$.

The observations presented in this work are also in good agreement with a
recent study of cluster galaxies in the EAGLE simulations, where Troncoso-
Iribarren et al. (2020) have shown that properties such as the SFR, star
formation efficiency and ISM pressure are enhanced on the leading edge of the
normal star-forming galaxies. On the other hand, an increase in the gas
particles is observed on the ‘trailing edge’ of these galaxies, suggesting
removal of cold gas via RPS. Similar results were obtained by Boselli et al.
(2021), who presented hydrodynamical simulations of the RPS galaxy IC 3476
along with its multi-wavelength data. The fact that UGC 10420 seems to have
more gas present on the trailing edge (Fig. 7), and an asymmetric distribution
of star-forming regions, supports the results from the simulations.

These results from simulations were recently tested observationally by Roberts
et al. (2022b), who found them to agree with the resolved analysis of the
integral field spectroscopic data of 29 jellyfish galaxies. A case study of IC
3949 presented by these authors is further evidence in favour of a scenario
where the increased ISM pressure on the leading edge compresses the atomic
Hydrogen and turns it into molecular gas, thereby triggering a localized burst
of star formation. Troncoso-Iribarren et al. (2020) also showed that this
effect is most pronounced in galaxies in the stellar mass range of
$10^{9.5}-10^{10.5}~{}M_{\odot}$, which conveniently includes UGC 10420 (Table
4).

An examination of the individual XUV star-forming regions (defined in Sec.
3.2) shows that they are statistically brighter than their counterparts at
lower galactocentric distances, and have relatively bluer FUV-NUV colours and
lower SFR. These observations are in agreement with the results of Werk et al.
(2010), who analysed the HI and FUV data for some nearby star-forming
galaxies. Werk et al. (2010) found that 8%–11% of emission-line point sources,
near star-forming galaxies in their sample, are HII regions associated with
the extended UV disk of the galaxies.

Any environmental mechanism which influences the gas content of a galaxy,
thereby affecting its SFR, can potentially impact the AGN activity as well. In
order to test this hypothesis, Peluso et al. (2022) have recently exploited
the integral field data for 115 RPS galaxies from MANGA and MUSE. Peluso et
al. (2022) find that AGN fraction among RPS galaxies is higher than their non-
RPS counterparts. Furthermore, the incidence of optical AGN (classifiable
using the BPT diagnostics) is $51\%$ among massive ($M^{*}\geq
10^{10}M_{\odot}$) RPS galaxies. It therefore comes as no surprise that UGC
10420 is optically classified as a LINER (Toba et al., 2014). On the contrary,
evidence has been presented in the literature to show that presence of a low-
ionization emission region may not always correspond to nuclear activity (e.g.
Belfiore et al., 2016). Interested readers are directed to Boselli et al.
(2022, and references therin), for a detailed discussion on the subject, while
deeper and high resolution data would be required to confirm presence of AGN
in UGC 10420.

Analysis of archival X-ray data shows that UGC 10420 lies just at the edge of
the X-ray emitting region of Abell 2199. Two bright X-ray sources, a few tens
of kpc away from the centre of the galaxy without any optical counterpart are
clearly visible, along with very faint emission from the central region of the
galaxy. Such bright sources (hot spots, hereafter), are reminiscent of those
generally observed around bright active galactic nuclei like Pictor A.
Although such hot spots are often connected with a jet seen as faint diffuse
emission (Hardcastle et al., 2016), such is not the case with UGC 10420. The
eastern hot spot appears to be embedded in diffuse radio emission at that
location as has been seen in Pictor A (Thimmappa et al., 2021). It should be
noted that the nucleus in Pictor A is about 20 times brighter than the hot
spots (Hardcastle et al., 2016), while almost the reverse is true here.

The X-ray spectrum of the two hot spots in UGC 10420 are well fitted by a
power-law with photon index of $1.8^{+0.3}_{-0.2}$ and $1.6\pm{0.2}$ for the
eastern and western source, respectively. The luminosities of these hot spots
are similar to the hot spots in Pictor A, while the nucleus is an order of
magnitude weaker. If confirmed with deeper Chandra observations with higher
resolution, this would be the first case of hot spots associated with such a
weak nucleus. This also indicates that we do not find any evidence of
enhancement in the nuclear activity in the galaxy due to the RPS process,
which has a luminosity typical of low-activity nucleus in LINERS.

A careful analysis of diffuse X-ray emission indicates that the hot galactic
plasma in UGC 10420 has a temperature of $0.24^{+0.09}_{-0.06}$ keV,
consistent with that observed in spiral galaxies (e.g. Li et al., 2008; Mineo
et al., 2012). Also, the X-ray luminosity of the diffuse gas component in UGC
10420 is $1.8\pm{0.9}\times 10^{40}$ erg s-1 (0.4–2.0 keV), which is typical
of spiral galaxies (Tyler et al., 2004; Owen & Warwick, 2009; Mineo et al.,
2012). This also indicates that the RPS has no effect on the hot gas in the
galaxy.

In a nutshell, multi-wavelength analysis of UGC 10420 confirms that it is a
RPS galaxy which is undergoing a short-lived phase of intense star formation,
as it interacts with the ICM in the cluster Abell 2199. While the star-forming
knots on the western side of the disk are formed as a consequence of the
compression of ISM of the galaxy due to RPS, the star formation on the eastern
side is part of the wake which comprises loosely bound or ejected gas from the
galaxy. References from the literature suggest that deep narrow-band and radio
continuum imaging of UGC 10420 should produce further evidence to support the
ideas presented in this paper. Although it is worth mentioning that UGC 10420
is unique not only because of the asymmetric distribution of star-forming
regions, but also due to its status as an XUV disk galaxy hosted by a cluster.

##  5 Epilogue

Although the multi-wavelength analysis of the data for UGC 10420 has thrown
some light on the evolution of this and such similar objects, it is worth
mentioning the paucity of narrow-band data. We believe narrow-band imaging
(H$\alpha$), sensitive to the presence of massive O stars would be a key to
probing the XUV star-formation in this galaxy. Also, continuum and HI
emission, and molecular gas observations can throw light on the distribution
of gas in and around the galaxy, and may prove very helpful in understanding
the role of RPS in the evolution of UGC 10420, just like other RPS galaxies
observed in clusters (e.g. Smith et al., 2010; Werk et al., 2010; Cortese et
al., 2007; Yagi et al., 2010; Roman-Oliveira et al., 2019; Boselli et al.,
2021).

##  6 Acknowledgements

S. Mahajan was funded by the SERB Research Scientist (SRS) award (SB-
SRS/2020-21/56/PS), Department of Science and Technology (DST), Government of
India. Kulinder Pal Singh thanks the Indian National Science Academy for
support under the INSA Senior Scientist Programme. Authors are grateful to Dr.
Dharam Vir Lal for his help with the LOFAR data. We are grateful to the
anonymous reviewer and the associate editor for their constructive criticism
which helped in improving the readability of this manuscript.

This publication uses data from the AstroSat mission of the Indian Space
Research Organisation (ISRO), archived at the Indian Space Science Data Centre
(ISSDC). UVIT project is a result of collaboration between IIA (Bengaluru),
IUCAA (Pune), TIFR (Mumbai), several centres of ISRO, and the Canadian Space
Agency (CSA). This research has made use of the NASA/IPAC Infrared Science
Archive, which is funded by the National Aeronautics and Space Administration
and operated by the California Institute of Technology. The topcat software
(Taylor, 2005) was used for some of the analysis presented in this paper. This
publication makes use of data products from the Wide-field Infrared Survey
Explorer, which is a joint project of the University of California, Los
Angeles, and the Jet Propulsion Laboratory/California Institute of Technology,
funded by the National Aeronautics and Space Administration. This dataset or
service is made available by the Infrared Science Archive (IRSA) at IPAC,
which is operated by the California Institute of Technology under contract
with the National Aeronautics and Space Administration. We acknowledge the use
of LOFAR data in accordance with the credits given on https://lofar-
surveys.org/credits.html, and SDSS data given on
https://www.sdss.org/collaboration/citing-sdss/. The X-ray data were
downloaded from the High Energy Astrophysics Science Archive Research Center
(HEASARC), maintained by NASA’s Goddard Space Flight Center. This research has
made use of SAOImageDS9, developed by Smithsonian Astrophysical Observatory,
and the HEASoft FTOOLS (http://heasarc.gsfc.nasa.gov/ftools).

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