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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel  17137, 17138, 17139
Message-Id: <20250408071702.2317E288079C@server.astronomerstelegram.org>
Date: Tue,  8 Apr 2025 03:17:02 -0400 (EDT)

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ATEL #17137							     ATEL #17137

Title:	Swift J001159.1+522440: FTW optical observations
Author:	Malte Busmann (LMU), Brendan O&#39;Connor (Carnegie Mellon
		U.), Daniel Gruen (LMU), and Antonella Palmese (Carnegie Mellon U.)
Queries:	m.busmann@physik.lmu.de,boconno2@andrew.cmu.edu
Posted:	7 Apr 2025; 13:06 UT
Subjects:Optical, X-ray, Transient

We observed the UV and X-ray transient Swift J001159.1+522440 (Evans et
al., ATel #17128) with the Three Channel Imager (3KK) at the Fraunhofer
Telescope at Wendelstein Observatory (FTW) in the g r and z band. We took
14 x 180 s exposures in the r and g band starting at 2025-04-05T02:07:04
and 2025-04-05T02:42:26 respectively. In parallel, we obtained 28 x 180
s exposures in the z band. We detect the source at:

g ~ (20.00 +/- 0.03) mag 
r ~ (19.53 +/- 0.02) mag 
z ~ (18.74 +/- 0.02) mag

which is significantly brighter than the archival PS1 magnitudes of g~21.1
mag, r~19.8 mag and z~18.8 mag. In the difference imaging with templates
from PS1 we detect it at:

g ~ (20.26 +/- 0.05) mag 
r ~ (20.28 +/- 0.05) mag 
z ~ (19.22 +/- 0.07) mag

with no visible offset from the underlying source.

The magnitudes are calibrated against the PS1 catalog and not corrected
for Galactic extinction.

We thank Michael Schmidt from the Wendelstein Observatory staff for obtaining
these observations.

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Password Certification: Malte Busmann (m.busmann@physik.lmu.de)
https://www.astronomerstelegram.org/?read=17137
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ATEL #17138							     ATEL #17138

Title:	Swift observations of SN 2025coe, a potential Ca-rich SN Ib
Author:	T. S. Hu, S. Ketchum, V. Tananko, D. Byun, X. Xiang, J. M.
		Miller (University of Michigan)
Queries:	jonmm@umich.edu
Posted:	7 Apr 2025; 20:50 UT
Subjects:Optical, Ultra-Violet, Supernovae, Transient

We report on recent Swift UVOT observations of SN 2025coe, recently classified
as a potential Ca-rich SN Ib (Andrews et al. 2025).  This class of supernovae
is notable for particularly rapid increases and decreases to and from peak
flux levels, and for spectra that are dominated by Ca at late times.  It
is possible that double-white dwarf binaries, or white dwarf plus neutron
star binaries, are the progenitors of Ca-rich SN Ib.

We analyzed a set of 9 UVOT observations, spanning MJD 60732-60751.  In
the W2 filter, the measured flux density on MJD 60732 is F_nu = 5.9 +/-
0.2 E-15 erg/cm2/s/A, falling to F_nu = 0.96 +/- 0.05 E-15 two days later
on MJD 60734.  The UVOT M2 filter has the smallest red leak, and in this
band the flux density falls from F_nu = 4.9 +/- 0.2 E-15 erg/cm2/s/A to
F_nu = 0.8 +/- 0.1 E-15 erg/cm2/s/A over the same two days.  Apart from
the V band, which shows a relatively steady flux at all times, the other
UVOT bands show similarly sharp declines, and all bands appear to reach
a quasi-steady flux level by 60742, just 10 days after the initial UVOT
exposure.

Further photometry and spectroscopy are encouraged at all wavelengths.

References:

Andrews, M., et al., 2025, TNSCR 1033

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Password Certification: Jon Miller (jonmm@umich.edu)
https://www.astronomerstelegram.org/?read=17138
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ATEL #17139							     ATEL #17139

Title:	Swift observations of the new outburst of the BH transient
		4U 1630-472
Author:	Melania Del Santo, Alberto Segreto, Carlotta Miceli (INAF/IASF
		Palermo)
Queries:	melania.delsanto@inaf.it
Posted:	7 Apr 2025; 23:28 UT
Subjects:X-ray, Black Hole, Transient

In the last 10 days, the BH transient 4U 1630-472 has been showing signs
of increased activity in the Swift/BAT survey data.  
Therefore, we triggered a monitoring campaign with Swift which observed
the source on 2025-04-06 (XRT exposure 1.2 ks) and on 2025-04-07 (XRT exposure
1.1 ks). These two observations are consistent in the spectral shape and
flux.

We simultaneously fitted the BAT hard X-ray spectrum (15-120 keV) stacked
from 2025-03-31 to 2025-04-07 and the XRT spectrum (0.5-10 keV) taken on
April 7th with an absorbed thermal Comptonisation model. The best fit results
in an absorption column density of N_H=9.4 (+1.3/-1.1) cm^-2, an electron
temperature of 30 (+11/-5) keV, a power-law index of 1.65 +/-0.06. Thus,
the spectral parameters are consistent with 4U 1630-472 being in the hard
state, which is rarely observed in this source.

The estimated absorbed fluxes in the 1-10 keV and 15-100 keV energy bands
are roughly 9.3E-10 erg/cm^2/s and 3.4E-9 erg/cm^2/s, respectively.

Future Swift observations are planned in the upcoming days to monitor the
outburst evolution. We thank the Swift team for assistance and the quick
planning of the observations.

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Password Certification: Melania Del Santo (melania@ifc.inaf.it)
https://www.astronomerstelegram.org/?read=17139
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