文件操作 - 1757315479.M972490P1125.mail.planetcloud-host.com,S=7823,W=7960:2,

文件: /var/vmail/bicar.it/stefano/cur/1757315479.M972490P1125.mail.planetcloud-host.com,S=7823,W=7960:2,

编辑文件内容

Received-SPF: Pass (sender SPF authorized) identity=mailfrom; client-ip=174.142.199.243; helo=server.astronomerstelegram.org; envelope-from=atel@astronomerstelegram.org; receiver=stefano@bicar.it 
To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel 17375, 17376
Message-Id: <20250908071116.16F14288087D@server.astronomerstelegram.org>
Date: Mon, 8 Sep 2025 03:11:16 -0400 (EDT)

------------------------------------------------------------------------------ 
The Astronomer's Telegram is free to read, free to publish, free to
use.  Thanks to the support of our patrons, we can continue to
keep it free. https://www.patreon.com/astronomerstel
------------------------------------------------------------------------------ 
The Astronomer's Telegram                   http://www.astronomerstelegram.org 
------------------------------------------------------------------------------
Posted: Within the last 24 hours
==============================================================================
ATEL #17375							     ATEL #17375

Title:	XRISM/Xtend Transient Search (XTS) detected an X-ray flare
		possibly from a YSO
Author:	M. Yoshimoto (Ehime U.), T. Kiyomoto (Saitama U.), K. Fukushima,
		Y. Kanemaru, S. Ogawa, Y. Uchida, T. Yoneyama (JAXA), M. Audard (U.
		de Geneve), E. Behar (Technion), T. Hakamata (UOsaka), S. Inoue (Kyoto
		U.), Y. Ishihara (Chuo U.), C. Kang (Ehime U.), T. Kohmura (TUS),
		H. Kuramoto (UOsaka), J. Kurashima (U. of Miyazaki), Y. Maeda (JAXA),
		H. Matsumoto (UOsaka), T. Matsushima (U. of Miyazaki), A. Miyamoto
		(UOsaka), 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.), Y. Sakamoto (Tohoku U.), M. Shidatsu (Ehime
		U.), H. Sugai (Chuo U.), H. Takahashi (Hiroshima U.), T. Takagi (Ehime
		U.), S. Takatuska (UOsaka), R. Takemoto (U. of Miyazaki), Y. Terada
		(Saitama U.), Y. Terashima (Ehime U.), Y. Tsuboi (Chuo U.), H. Uchida
		(Kyoto U.)
Queries:	tyoneyama263@g.chuo-u.ac.jp
Posted:	7 Sep 2025; 10:05 UT
Subjects:X-ray, Star, Transient, Young Stellar Object

XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray
source XRISM J1044-5941 on 2025-09-05 TT. The source position is determined
to be (R.A., Dec.) = (160.944, -59.678), with a systematic error of &sim;
40 arcsec. One of the plausible counterparts is a Young Stellar Object
2MASS J10434657-5940394, which is located &sim; 1 arcsec apart from the
position of XRISM J1044-5941. Plausible X-ray counterparts are 2CXO J104346.5-594038,
4XMM J104348.9-594031.  All statistical uncertainties in this report are
provided as a 90% confidence level unless stated otherwise.

The flare started at 2025-09-05 at &sim; 02:12 TT. The flare reached its
peak on 2025-09-05 at &sim; 02:27. The flare exponentially decayed in 1.1
(+0.4/-0.2) &times; 104 sec.

The peak flux is calculated as 1.3 (+0.1/-0.6) &times; 10-12
erg s-1 cm-2 (1.0 &ndash; 10.0 keV). A systematic
error of roughly 20% should be added to the statistical error. The corresponding
luminosity is 5.0 (+0.4/-2.3) &times; 1032 erg s-1
by assuming the distance to XRISM J1044-5941 of 1.8 kpc.

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.

------------------------------------------------------------------------------
Password Certification: Tomokage Yoneyama (tyoneyama263@g.chuo-u.ac.jp)
https://www.astronomerstelegram.org/?read=17375
==============================================================================
ATEL #17376							     ATEL #17376

Title:	Broadband radio flaring of the FSRQ PKS 1725+123 from 2 to
		22 GHz
Author:	Yu. V. Sotnikova, T. V. Mufakharov, A. K. Erkenov, T. A. Semenova
		(SAO RAS), Tao An (SHAO CAS), M. A. Kharinov (IAA RAS)
Queries:	timur.mufakharov@gmail.com
Posted:	7 Sep 2025; 11:31 UT
Subjects:Radio, Millimeter, Optical, Gamma Ray, TeV, AGN, Quasar

We report significant cm-band radio brightening of the flat-spectrum radio
quasar (FSRQ) PKS 1725+123 observed with the RATAN-600 and RT-32 radio
telescopes. This follows the recent enhanced activity in &gamma-rays (ATel
#17316 and #17370), optical (ATel #17345), mm-band radio (ATel #17356),
and, for the first time, in the VHE band with MAGIC (ATel #17344) during
July-August 2025. PKS 1725+123 is a low-synchrotron-peaked blazar with
a one-sided milli-arcsecond-scale jet, now detected at VHE, exhibiting
prominent multiband variability and considered a candidate neutrino emitter
since IceCube event IC201021A.

On 2025 August 25, we measured flux densities of PKS 1725+123 at five
frequencies using the RATAN-600 telescope, obtaining the following values
(in Jy):

1.18 &plusmn; 0.25 at 22.3 GHz</li>
0.67 &plusmn; 0.06 at 11.2 GHz</li> 
0.62 &plusmn; 0.06 at 8.2 GHz</li> 
0.48 &plusmn; 0.04 at 4.7 GHz</li>
0.35 &plusmn; 0.02 at 2.3 GHz</li>

Additional measurements were carried out with the radio telescopes RT-32
in Zelenchukskaya and Badary observatories (Institute of Applied Astronomy,
Russian Academy of Sciences, https://iaaras.ru/en/quasar/) during the sessions
on 2025 August 23, 24 and 30. The obtained flux density at 5.05 GHz is
0.55 &plusmn 0.03 Jy on August 23, and 0.53 &plusmn 0.04 Jy on August 24.
At 8.63 GHz we obtained the flux density of 0.81 &plusmn 0.03 Jy on August
23, and 0.77 &plusmn 0.04 Jy on August 30.

<a href="https://rat.sao.ru/scientific-results/broadband-radio-flaring-of-the-fsrq-pks-1725-123-from-2-to-22-ghz/">Figures
1 and 2</a> illustrate the long-term radio light curves in 2017-2025 and
broadband spectra of PKS 1725+123 including the recent RATAN-600 and RT-32
measurements and archival data, highlighting the current flaring episode.
The spectral shape remains inverted with the median spectral index value
of +0.30 (0.05) at 2.3-22.3 GHz (S ~ &nu &alpha).

------------------------------------------------------------------------------
Password Certification: Timur Mufakharov (timur.mufakharov@gmail.com)
https://www.astronomerstelegram.org/?read=17376
==============================================================================

==============================================================================
This is an automatically-generated notice.  You can remove yourself permanently
from receiving both the Daily Email Digest and Instant Email Notices from
The Astronomer's Telegram by following this link:
https://www.astronomerstelegram.org?unsubscribe&confirmation=a803d34e7ea924f9a4142bac00763549&address=stefano@bicar.it

文件操作 - 1757315479.M972490P1125.mail.planetcloud-host.com,S=7823,W=7960:2,

文件: /var/vmail/bicar.it/stefano/cur/1757315479.M972490P1125.mail.planetcloud-host.com,S=7823,W=7960:2,

编辑文件内容

修改文件时间

删除文件