文件操作 - 1761376345.M565538P2023.mail.planetcloud-host.com,S=8128,W=8263:2,

文件: /var/vmail/bicar.it/stefano/cur/1761376345.M565538P2023.mail.planetcloud-host.com,S=8128,W=8263:2,

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 17452, 17453
Message-Id: <20251025071222.2A92B28808B2@server.astronomerstelegram.org>
Date: Sat, 25 Oct 2025 03:12:22 -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 #17452							     ATEL #17452

Title:	Fermi-LAT detection of enhanced gamma-ray activity from the
		FSRQ PKS 0215+015
Author:	P. Monti-Guarnieri (University of Trieste and INFN Trieste),
		E. Bissaldi (Politecnico and INFN Bari), A. Holzmann Airasca (University
		of Trento and INFN Bari), G. La Mura (INAF - Astronomical Observatory
		of Cagliari), S. Lopez-Perez (LLR, Ecole Polytechnique &amp; CNRS/IN2P3),
		on behalf of the Fermi Large Area Telescope Collaboration
Queries:	pietro.monti-guarnieri@phd.units.it
Posted:	24 Oct 2025; 15:05 UT
Subjects:Gamma Ray, >GeV, Blazar, Quasar

The Large Area Telescope (LAT), one of the two instruments on the Fermi
Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from
a source positionally consistent with the flat-spectrum radio quasar PKS
0215+015, also known as 4FGL J0217.8+0144 (Abdollahi et al. 2022, ApJS,
260, 53), with coordinates R.A. = 34.45398 deg, Dec. = +1.74714 deg (J2000;
Le Bail et al., 2016, AJ, 151, 79), and redshift z=1.715 (Boisse et al.,
1988, A&A, 192, 1-8).

Preliminary analysis indicates that this source was in an elevated gamma-ray
emission state on October 23, 2025, with a daily averaged gamma-ray flux
(E>100MeV) of (0.7+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty
only). This corresponds to a flux increase of a factor of 15 relative to
the average flux reported in the fourth data release of the fourth Fermi-LAT
catalog (4FGL-DR4, Ballet et al. 2023, arXiv:2307.12546). This is the highest
LAT daily flux ever observed for this source. The corresponding photon
index is 1.5+/-0.1, indicating a significantly harder spectrum than the
one corresponding to the 4FGL-DR4 value of 2.18+/-0.01. The highest-energy
photon associated with the source at a probability p>0.999 had an energy
of 25 GeV, and was recorded at 06:35:50.096 UTC on 2025-10-23.

Because Fermi normally operates in an all-sky scanning mode, regular gamma-ray
monitoring of this source will continue. A preliminary light curve for
PKS 0215+015 can be accessed via the Fermi-LAT Light-Curve Repository at
<a href="https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.html?source_name=4FGL_J0217.8+0144">https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.html?source_name=4FGL_J0217.8+0144</a>.
We encourage multifrequency observations of this source. For this source,
the Fermi-LAT contact person is Pietro Monti-Guarnieri (pietro.monti-guarnieri@phd.units.it).

The Fermi-LAT is a pair conversion telescope designed to cover the energy
band from 20 MeV to greater than 300 GeV. It is the product of an international
collaboration between NASA and DOE in the U.S. and many scientific institutions
across France, Italy, Japan and Sweden.

------------------------------------------------------------------------------
Password Certification: Giovanni La Mura (giovanni.lamura@inaf.it)
https://www.astronomerstelegram.org/?read=17452
==============================================================================
ATEL #17453							     ATEL #17453

Title:	XRISM/Xtend Transient Search (XTS) detected an X-ray flare
		from Pul -3  540245
Author:	S. Takatuska (UOsaka), H. Matsumoto (UOsaka), 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. Kiyomoto (Saitama
		U.), T. Kohmura (TUS), H. Kuramoto (UOsaka), J. Kurashima (U. of Miyazaki),
		Y. Maeda (JAXA),  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.),  R. Takemoto (U. of Miyazaki), Y. Terada (Saitama U., JAXA),
		Y. Terashima (Ehime U.), Y. Tsuboi (Chuo U.), H. Uchida (Kyoto U.),
		M. Yoshimoto (Ehime U.), S. Ueda (Kanazawa U.)
Queries:	matumoto@ess.sci.osaka-u.ac.jp
Posted:	25 Oct 2025; 03:32 UT
Subjects:X-ray, Star, Transient

XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray
source XRISM J0915+4102on 2025-10-21 TT. The source position is determined
to be (R.A., Dec.) = (138.787, 41.035), with a systematic error of &sim;
40 arcsec. One plausible counterpart is Pul -3  540245 which corresponds
to an infrared source 2MASS J09150912+4101386. Pul -3 540245 is located
&sim; 27arcsec apart from the position of XRISM J0915+4102.

The observation began at 2025-10-21 at &sim; 04:02. The flare was already
active at that time. The flare reached its peak on 2025-10-21 at &sim;
05:42.

The peak flux is calculated as 9 &times; 10-13 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 2 &times; D1300pc2 &times; 1031 erg
s-1 by assuming the distance to XRISM J0915+4102 of D1300pc.

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: Hironori Matsumoto (matumoto@ess.sci.osaka-u.ac.jp)
https://www.astronomerstelegram.org/?read=17453
==============================================================================

==============================================================================
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 - 1761376345.M565538P2023.mail.planetcloud-host.com,S=8128,W=8263:2,

文件: /var/vmail/bicar.it/stefano/cur/1761376345.M565538P2023.mail.planetcloud-host.com,S=8128,W=8263:2,

编辑文件内容

修改文件时间

删除文件