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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel 17793, 17794
Message-Id: <20260512070520.CFCF828807D2@server.astronomerstelegram.org>
Date: Tue, 12 May 2026 03:05:20 -0400 (EDT)

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Posted: Within the last 24 hours
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ATEL #17793							     ATEL #17793

Title:	Spectroscopic Classifications of Optical Transients with Keck
		II/KCWI
Author:	Jenna Karcheski, Kishore C. Patra, Ryan J. Foley (UCSC)
Queries:	kcpatra@ucsc.edu
Posted:	11 May 2026; 10:35 UT
Subjects:Optical, Supernovae, Transient

We report the following classifications of optical transients from spectroscopic
observations with the Keck Cosmic Web Imager (KCWI) Integral Field Spectrograph.
The targets were supplied by the Legacy Survey of Space and Time (LSST)
via the ANTARES alerts broker (Matheson et al., 2021, AJ, 161, 107). Observations
were made on 2026 May 7 UT. Classifications were performed with SNID (Blondin
& Tonry, 2007, ApJ, 666, 1024).

Name        	                | IAU Name  	| RA (J2000)  | Dec (J2000)	|
z	| Type	   | Phase | Notes 
LSST-AP-DO-170257199649521669   | AT2026kfw	| 09:56:52.77 | +01:49:59.20	|
0.21	| SN Ia	   | +7 d  |(1) 
LSST-AP-DO-170230797176406143   | AT2026jkr	| 10:04:17.29 | +03:25:22.88	|
0.35	| SN Ic-BL | +3 d  | 
LSST-AP-DO-170226393328648251   | AT2026ikn	| 09:59:46.48 | +03:46:48.85	|
0.298	| SN Ia    | +15 d |(2)

Notes: 
When the redshift is given to 2 decimal places, it is derived from the
SN spectrum.  Otherwise, the redshift is determined from the host galaxy.

(1) We measure Si II 6355 velocity of  -12,500 km/s.  
(2) Redshift was determined using emission lines from the host galaxy.
The spectrum is highly contaminated by galaxy light.  SNID template fitting
was performed after subtracting a host-galaxy template spectrum. The best-fit
match was SN 2005hf at +15 days past peak brightness.

We thank the Vera C. Rubin Observatory leadership and staff, and especially
thank the Prompt Processing team (Findeisen et al., arXiv:2603.19541),
for publicly releasing these discoveries.

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Password Certification: Kishore Patra (kcpatra@ucsc.edu)
https://www.astronomerstelegram.org/?read=17793
==============================================================================
ATEL #17794							     ATEL #17794

Title:	Title: XRISM/Xtend Transient Search (XTS) detected an X-ray
		brightening from XRISM J0602-4006
Author:	A. Miyamoto (UOsaka), K. Fukushima (TUS), Y. Kanemaru, A.
		Miyamoto, Y. Omiya, 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), Y. Maeda (JAXA), H. Matsumoto
		(UOsaka), M. Mizumoto (UTEF), Y. Motogami (Saitama U.), T. Narita
		(RIKEN), M. Nobukawa (NUE), H. Noda (Tohoku U.), S. Ogawa (TUS), Y.
		Sakamoto (Tohoku U.), M. Shidatsu (Ehime U.), H. Takahashi (Hiroshima
		U.), T. Takagi (Ehime U.), S. Takatsuka (UOsaka), F. Takisawa (Ehime
		U.), Y. Terada (Saitama U., JAXA), Y. Terashima (Ehime U.), Y. Tsuboi
		(Chuo U.), H. Uchida (Kyoto U.), A. Yoshimoto (NWU), M. Yoshimoto
		(Ehime U.)
Queries:	kxfukushima@gmail.com
Posted:	11 May 2026; 14:03 UT
Subjects:X-ray, Star

XRISM/Xtend Transient Search (XTS) identified an additional X-ray transient
from the source XRISM J0602-4006, potentially corresponding to 2CXO J060212.4-400619
(ATel #17785), on 2026-05-10 TT. A plausible counterpart is the star UCAC2
14546266 with a distance of &sim; 1.3 kpc.

The brightening lasted from 2026-05-10 at &sim; 08:19 TT to 2026-05-10
at &sim; 15:16. The peak flux is calculated as 1 &times; 10-12
erg s-1 cm-2 (0.4 &ndash; 10.0 keV). A systematic
error of roughly 20% should be taken into account. The corresponding luminosity
is 2 &times; 1032 erg s-1 by assuming the distance
to XRISM J0602-4006 of 1.3 kpc. The peak luminosity is approximately twice
that of the previous brightening reported in ATel #17785.

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
and their corresponding counterparts in the same field of view.

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Password Certification: Kotaro Fukushima (kxfukushima@gmail.com)
https://www.astronomerstelegram.org/?read=17794
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