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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel 17241, 17242
Message-Id: <20250624070940.3843828807D7@server.astronomerstelegram.org>
Date: Tue, 24 Jun 2025 03:09:40 -0400 (EDT)

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Posted: Within the last 24 hours
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ATEL #17241							     ATEL #17241

Title:	GIT observations of AT 2025nsa in M31
Author:	Shatakshi Chamoli (IIA), Judhajeet Basu (IIA), Sudhanshu Barway
		(IIA), G. C. Anupama (IIA), Aditya Pawan Saikia (IITB), Varun Bhalerao
		(IITB) and GIT Team
Queries:	shatakshi.chamoli@iiap.res.in
Posted:	23 Jun 2025; 12:41 UT
Subjects:Optical, Cataclysmic Variable, Nova, Transient

We report optical photometric observations
of the nova <a href="https://www.wis-tns.org/object/2025nsa">AT 2025nsa</a> (R.A. = 00:42:17.341, DEC= +41:08:55.23, Discovery Date: 2025-06-17.1498)
by the GROWTH-India Telescope (GIT). This nova was discovered by GOTO group
and reported on TNS. Claudio Balcon classified it as a nova in its Fe ll
phase, noting prominent Balmer lines and the characteristic &ldquo;Fe II
forest&rdquo; emission (classification reported on TNS).

The nova was detected across g&rsquo;,
r&rsquo;, i&rsquo; and z&rsquo; bands in 360s exposure frames. The PSF
photometry magnitudes (AB),&nbsp; calibrated against PanSTARRS DR1 (Chambers
et al., 2016) and not corrected for Galactic extinction are:

Obs date (UTC)&nbsp; |filter | Mag &plusmn;
error (AB)&nbsp;

We note that the nova is brighter in the
redder bands. Follow-up observations are being undertaken to understand
the nature of this object.

&nbsp;

The GROWTH-India Telescope (GIT; Kumar
et al. 2022) is a 70-cm telescope with a 0.7-degree field of view, set
up by the Indian Institute of Astrophysics (IIA) and the Indian Institute
of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. It is
located at the Indian Astronomical Observatory (Hanle), operated by IIA.
We acknowledge funding by the IITB alumni batch of 1994, which partially
supports the operations of the telescope. Telescope technical details are
available at <a href="https://sites.google.com/view/growthindia/">https://sites.google.com/view/growthindia/</a>.

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Password Certification: Judhajeet Basu (judhajeet.basu@iiap.res.in)
https://www.astronomerstelegram.org/?read=17241
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ATEL #17242							     ATEL #17242

Title:	XRISM/Xtend Transient Search (XTS) detected an X-ray flare
		from TWA 11
Author:	H. Sugai (Chuo U.), K. Fukushima, Y. Kanemaru, S. Ogawa (JAXA),
		M. Audard (U. de Geneve), E. Behar (Technion), T. Hakamata (Osaka
		U.), S. Inoue (Kyoto U.), Y. Ishihara (Chuo U.), C. Kang (Ehime U.),
		T. Kiyomoto (Saitama U.), T. Kohmura (TUS), H. Kuramoto (Osaka U.),
		J. Kurashima (U. of Miyazaki), Y. Maeda (JAXA), H. Matsumoto (Osaka
		U.), T. Matsushima (U. of Miyazaki), A. Miyamoto (Osaka U.), M. Mizumoto
		(UTEF), K. Mori (U. of Miyazaki), Y. Motogami (Saitama U.), N. Nagashima
		(Chuo U.), T. Narita (Kyoto U.), M. Nobukawa (NUE), H. Noda (Tohoku
		U.), K. Pottschmidt (UMBC, NASA GSFC, CRESST), Y. Sakamoto (Tohoku
		U.), M. Shidatsu (Ehime U.), H. Takahashi (Hiroshima U.), T. Takagi
		(Ehime U.), S. Takatuska (Osaka U.), R. Takemoto (U. of Miyazaki),
		Y. Terada (Saitama U.), Y. Terashima (Ehime U.), Y. Tsuboi (Chuo U.),
		H. Uchida (Kyoto U.), T. Yoneyama (Chuo U.), M. Yoshimoto (Ehime U.)
Queries:	CorrespondingAuthor&#39;sEmailAddress
Posted:	23 Jun 2025; 13:46 UT
Subjects:X-ray, Binary, Star, Transient, Young Stellar Object

XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray
source XRISM J1236-3952 on 2025-06-22 TT. The source position is determined
to be (R.A., Dec.) = (189.005, -39.874), with a systematic error of &sim;
40 arcsec. A plausible counterpart is a Young Stellar Object Candidate
TWA 11 (HD 109573). TWA 11 is located &sim; 13 arcsec apart from the position
of XRISM J1236-3952 All statistical uncertainties in this report are provided
as a 90% confidence level unless stated otherwise.

The flare started at 2025-06-22 at &sim; 04:16 TT. The flare reached its
peak on 2025-06-22 at &sim; 05:09. The flare exponentially decayed in 4
&times; 103 sec.

This source also showed fluctuations in flux within a range of &sim; 10
times during the observation conducted the day before.

The peak flux is calculated as 1 &times; 10-11 erg s-1
cm-2 (0.4 &ndash; 10.0 keV). A systematic error of roughly 20%
should be added to the statistical error. The corresponding luminosity
is 8 &times; D70pc<sup2> &times; 1030 erg s-1
by assuming the distance to XRISM J1236-3952 of D67pc.

We derived the above systematic error for the flux by comparing our derived
values for the sources detected with XTS in several observations with those
for the corresponding X-ray counterparts. We estimated the systematic error
for the source position from the separations between the detected sources
with the corresponding counterparts in the same field of view.

&dagger; This telegram is dedicated to our wonderful colleague Katja Pottschmidt.

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Password Certification: Yohko Tsuboi (tsuboi@phys.chuo-u.ac.jp)
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