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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel  17716
Message-Id: <20260311070321.C70E028807A8@server.astronomerstelegram.org>
Date: Wed, 11 Mar 2026 03:03:21 -0400 (EDT)

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Posted: Within the last 24 hours
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ATEL #17716							     ATEL #17716

Title:	Optical follow-up of IGR J06074+2205
Author:	Roberto Nesci (INAF/IAPS), Mariateresa Fiocchi (INAF/IAPS),
		Antonio Vagnozzi (MPC589)
Queries:	roberto.nesci@inaf.it
Posted:	10 Mar 2026; 23:18 UT
Subjects:Optical, X-ray, Binary, Neutron Star, Variables

Nakajima et al. in ATel #17714 reported an X-ray alert from MAXI/GSC of
the HMXB IGR J06074+2205 with peak intensity on March 7 2026 at 0.030 c/s/cm2.
This epoch is in fair agreement with the expectation from the recurrence
period of 80 +/-2 days given by Mihara et al. in ATel #16351. 
According to our spectroscopic monitoring of the source with the S.Lucia
di Stroncone (MPC 589) 50 cm telescope, started in January 2024, the H-alpha
equivalent width (E.W.) emission has an oscillating behaviour with 570
days time scale, and was steadly decreasing since its maximum of -12 Angstrom
in September 2025 (see plot below). The E.W. on March 10 2026 is -6.9 Angstrom,
indicating a circumstellar disk of average extension: we would expect therefore
an X-ray outburst substantially fainter than those of September 2025 or
March 2024, when the H alpha E.W. was about -12 Angstrom.  
Using the MAXI on-demand system (https://maxi.riken.jp/mxondem/) we found
a count rate of 0.08 ph/s/cm2 in the strong outburst of March 2024 in the
2-6 keV band, and a similar value just before the peak of the strong outburst
of September 2025. Therefore, the relatively low value of 0.03 ph/s/cm2
of March 7 2026 is in fair agreement with the expectation from the H alpha
E.W., supporting the model that the interaction of the Pulsar with the
circumstellar disk of the Be star is the main cause of the X-ray outburst.

H alpha E.W. light curve: https://www.archiviomaffei.org/nesci/atel/halfa-xrt-plot.png
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