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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel  17838, 17839
Message-Id: <20260609070600.4A3EB288050A@server.astronomerstelegram.org>
Date: Tue,  9 Jun 2026 03:06:00 -0400 (EDT)

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Posted: Within the last 24 hours
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ATEL #17838							     ATEL #17838

Title:	TRAPPIST production rates of comet 220P/McNaught in outburst
Author:	E. Jehin, J. Manfroid, S. Hmiddouch, K. Aravind (STAR Institute,
		University of Liege)
Queries:	ejehin@uliege.ac.be
Posted:	8 Jun 2026; 18:55 UT
Subjects:Optical, Comet

The author reports that they obtained, using the TRAPPIST-North (Z53) telescope
located in Morocco, observations of comet 220P on the nights of June 4
and 5, a few days after a large outburst of -6 mag was reported (ATEL#17829).
They used broadband and cometary HB narrow-band filters (Farnham et al.
2000, Jehin et al. 2011) and computed preliminary production rates from
extracted profiles at 10.000 km using a Haser Model (Vp=Vd=0.85/SQRT(rh))km/s)
(Haser 1957). Zero Points were determined on close nights using standard
stars. The proxy to the dust production rate A(0)f(rho) was estimated by
profile fitting at 10.000 km (A'Hearn et al. 1984) and corrected for the
phase angle (Schleicher 2007).

220P/McNaught

Date UT=2026-06-05, rh= 1.56 au, Delta= 1.56 au, DT= -9 days

Q(OH)= 8.40 +/- 1.26 E27 s-1

Q(CN)= 3.04 +/- 0.45 E25 s-1

Q(C2)= 5.50 +/- 0.83 E25 s-1

A(0)f(rho)(Rc)= 2305 +/- 21 cm

220P/McNaught

Date UT=2026-06-06, rh= 1.56 au, Delta= 1.55 au, DT= -8 days

Q(OH)= 6.52 +/- 0.98 E27 s-1

Q(CN)= 2.27 +/- 0.34 E25 s-1

Q(C2)= 4.05 +/- 0.61 E25 s-1

A(0)f(rho)(Rc)= 1915 +/- 25 cm

The production rates have dropped significantly between the two nights.
The comet appears enriched in C2 with respect to CN. It also displays a
narrow and intense dust tail, visible in all filters and in in particular
in the dust continuum filters, which could indicate a fragmentation event.

Notations: rh= heliocentric distance (in au), Delta=geocentric distance
(in au), DT= Time to perihelion. OH, NH, C3, CN, and C2 are the HB gaseous
narrowband filters for the corresponding species, and BC, GC, and RC are
the blue, green and red dust continuum filters (Farnham et al. 2000).

Acknowledgments: TRAPPIST is a project funded by the Belgian F.R.S.-FNRS
under grant PDR T.0120.21 and the University of Liege. Observations were
carried out from the ESO La Silla Paranal and Oukaimeden Observatory. We
thank NASA, David Schleicher, and the Lowell Observatory for the loan of
the HB comet filters. https://www.trappist.uliege.be/

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Password Certification: Emmanuel Jehin (ejehin@uliege.be)
https://www.astronomerstelegram.org/?read=17838
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ATEL #17839							     ATEL #17839

Title:	Millimeter flaring in LEDA 66480/ESO 145-001 
Author:	Thomas Maccarone (Texas Tech University) on behalf of the
		South Pole Telescope consortium
Queries:	thomas.maccarone@ttu.edu
Posted:	8 Jun 2026; 19:02 UT
Subjects:Millimeter, AGN

The South Pole Telescope collaboration report millimeter flaring from SPT-SV
J211659.7-592000.  The source at this position has been marginally detected
in SPT data since 2021, with a mean flux density of 1.6+-0.5mJy at 90 GHz
and 1.9+-0.4 mJy at 150 GHz, and with ASKAP at about 9 mJy..  In the period
from 5/10-5/31, the source is at 5.8+-0.9 mJy with a highest measured value
in an individual epoch of 17 mJy and a test-statistic for variability of
51.2, corresponding to a >7-sigma variability detection.  The 150 GHz measurements
yield 6.7+-1.2 mJy over the same timespan, indicating a flat-to-mildly
inverted spectrum.

The source is associated with the nearby merging galaxy pair LEDA 66480/ESO
145-001, which is at redshift z=0.0605 (Jones et al. 2009MNRAS.399..683J),
or about 270 Mpc, assuming H0=70 km/sec/Mpc, but it is not clear which
member of the pair is the location of the flaring activity.  A ToO observation
on the Australia Telescope Compact Array has been triggered, but additional
follow-up at other wavelengths is encouraged.

The object has previously been seen in X-rays with eROSITA at a flux of
3.9e-14 erg/sec/cm^2(Merloni et al. 2024A&A...682A..34M ) and in the 4XMM
catalog with a flux of 5.5e-13 erg/sec/cm^2 (Webb et al. 2020A&A...641A.136W).
The spectrum appears to be strongly absorbed, so the difference between
the two values is likely to be at least partially because of the different
bandpasses.  Regardless, X-ray variability measurements would help understand
the source flaring, and the X-ray measurements suggest that the object
is a low luminosity AGN.

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Password Certification: Tom Maccarone (thomas.maccarone@ttu.edu)
https://www.astronomerstelegram.org/?read=17839
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