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From: atel@astronomerstelegram.org
Subject: ATel 17100, 17101
Message-Id: <20250323071115.DE5C22880532@server.astronomerstelegram.org>
Date: Sun, 23 Mar 2025 03:11:15 -0400 (EDT)

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Posted: Within the last 24 hours
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ATEL #17100							     ATEL #17100

Title:	FRB 20250316A: detection of a candidate associated X-ray source
		EP J120944.2+585060 by Einstein Probe
Author:	H. Sun, H. Q. Cheng, D. Y. Li, H. Y. Liu, C. C. Jin, Z. X.
		Ling, W. D. Zhang, Y. Liu (NAO, CAS), B. Zhang (UNLV), X. F. Wu, D.
		F. Hu, Y. Li, J. J. Geng (PMO, CAS), J. W. Hu, H. W. Pan, C. Zhang,
		L. Chen, S. Q. Jiang, Y. J. Song, T. Zhao (NAO, CAS), Y. Chen, C.
		K. Li, J. Guan, S. M. Jia, H. S. Zhao, J. Zhang, M. Y. Ge, W. W. Cui,
		H. Feng, W. Li, C. Z. Liu, F. J. Lu, L. M. Song, J. Wang, J. J. Xu,
		D. W. Han, S. N. Zhang, X. F. Zhao, Q. C. Zhao, Z. H. Yang, Q. C.
		Shui (IHEP, CAS), Q. C. Liu (THU), L. Piro (INAF), V. Burwitz, P.
		Friedrich, N. Meidinger, K. Nandra, A. Rau (MPE), J.-U. Ness, A. Santovincenzo
		(ESA), Nanda Rea (ICE-CSIC), P. O&#39;Brien (Univ. of Leicester),
		B. Cordier (CEA), W. Yuan (NAO, CAS) report on behalf of the Einstein
		Probe team:
Queries:	ep_ta@bao.ac.cn
Posted:	22 Mar 2025; 07:39 UT
Subjects:X-ray, Transient, Fast Radio Burst

We observed the field of the bright fast radio burst FRB 20250316A (Ng,
ATel #17081) with the Follow-up X-ray Telescope (FXT) on board the Einstein
Probe (EP) mission. A total of four observations were conducted. In the
first observation, which began at 2025-03-17T16:57:29(UTC) with an exposure
time of 2.9 ks, no X-ray sources were detected within 3 arcmin of the CHIME
position. In the second observation, starting at 2025-03-18T15:23:50(UTC)
with also 2.9 ks exposure, FXT detected a weak, uncatalogued X-ray source,
designated as EP J120944.2+585060. The position of this source is consistent
with the refined localization provided by CHIME (Leung, ATel #17086). The
unabsorbed X-ray flux is 3.4 x 10^-14 erg/cm2/s in the 0.5 - 10 keV band.

In the third observation starting at 2025-03-21T05:50:01(UTC) with an exposure
of 5.8 ks, the X-ray source was clearly detected at a flux consistent with
the previous level. The refined source position is RA = 182.4341 deg, Dec
= 58.8499 deg (J2000) with an uncertainty of 10 arcsec in radius (90% C.L.
statistical and systematic). This position remains consistent with the
CHIME localization, suggestive of EP J120944.2+585060 being likely associated
with the source of FRB 20250316A. Preliminary analysis of the forth observation,
taken 11 hours after the third one, shows a marginal trend of decrease
of the source flux, though the the telemetry data received is not complete
yet. Further analysis is ongoing. A Chandra DDT observation has been requested.

If EP J120944.2+585060 is indeed associated with FRB 20250316A and located
near the candidate host galaxy NGC 4141, which has a redshift of 0.0067
(Connor, ATel #17091), the inferred X-ray luminosity is approximately 3
x 10^39 erg/s in the 0.5 - 10 keV band during the EP observations.

Launched on January 9, 2024, EP is a space X-ray observatory to monitor
the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook
of X-ray and Gamma-ray Astrophysics). EP is a mission of the Chinese Academy
of Sciences in collaboration with ESA, MPE and CNES.

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Password Certification: Yuan Liu (liuyuan@bao.ac.cn)
https://www.astronomerstelegram.org/?read=17100
==============================================================================
ATEL #17101							     ATEL #17101

Title:	Swift XRT and UVOT Upper Limits of FRB 20250316A
Author:	Y. J. Yang, A. Aryan, T.-W. Chen (NCU), A. K. H. Kong (NTHU),
		T. Hashimoto (NCHU), R. Jin (NTTU)
Queries:	yjyang.astro@gmail.com
Posted:	22 Mar 2025; 16:32 UT
Subjects:Optical, X-ray, Fast Radio Burst

We report a pointed Swift observation (requested by Tohuvavohu) of the
field of FRB 20250316A (ATel #17081, #17082, #17084, #17086, #17090, #17091,
#17095, #17100). The observation was conducted on 2025-03-16 at 21:10:00
UTC, 12.6 hours after the first detection (Ng et al., ATel #17081), with
a total exposure time of approximately 5 ks.

No significant X-ray source was detected by XRT within the refined CHIME-KKO
localization region (Leung et al., ATel #17086). Using the method described
by Kraft et al. (1991), we estimated a 90% confidence level (CL) upper
limit for the count rate at 0.00046073 c/s. Assuming a photon index of
2 and NH = 1.43E+20 cm^-2 along the line of sight to the position (at z=0.0067;
Connor, ATel #17091), WebPIMMS predicts an unabsorbed flux of 1.300E-14
ergs cm^-2 s^-1 in the 0.5 - 10 keV band, which is consistent with the
flux level of EP J120944.2+585060 (Sun et al., ATel #17100).

No uncataloged optical counterpart consistent with the CHIME-KKO location
was detected in the UVOT observation, with a total exposure of 154.29 seconds
using the WHITE filter. A 3-sigma upper limit magnitude of >22.13 (AB system)
was obtained.

We thank the Swift team for scheduling the observation.

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Password Certification: Amar Aryan (amararyan941@gmail.com)
https://www.astronomerstelegram.org/?read=17101
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