Joint XMM/Chandra Accepted Cycle 14 Targets and Abstracts

Proposal Number	Subject Category	PI Name	Chandra Time	Title
14400003	BH AND NS BINARIES	Robin Barnard	5	A new heavyweight champion for stellar mass BHs? XMM and Chandra investigate
14500002	SN, SNR AND ISOLATED NS	Martino Marelli	50	Unveiling the pulsating behaviour of J1813-1246, a very energetic radio-quiet pulsar

Subject Category: BH AND NS BINARIES

Proposal Number: 14400003

Title: A new heavyweight champion for stellar mass BHs? XMM and Chandra investigate

PI Name: Robin Barnard

The X-ray source associated with the M31 globular cluster Bo 135 (hereafter XBo 135) may contain the largest stellar mass black hole to date. It has been observed several times with Chandra and XMM-Newton, and has always exhibited emission spectra characteristic of the black hole low state. XBo 135 exhibited this behaviour at ~4-6 E+38 erg/s, suggesting a primary mass >50 M_Sun. Possible formation scenarios include stellar mergers in the cluster center, or the direct collapse of a metal poor high mass star. We request 120 ks of XMM-Newton time to investigate the metalicity, and a 5 ks Chandra pointing to accurately locate the source.

Subject Category: SN, SNR AND ISOLATED NS

Proposal Number: 14500002

Title: Unveiling the pulsating behaviour of J1813-1246, a very energetic radio-quiet pulsar

PI Name: Martino Marelli

After 3 years Fermi has discovered dozens of new g-ray only pulsars. Such a discovery has far reaching implications for our overall understanding of pulsar physics. We propose a joint XMM-Chandra observation of J1813-1246, one of the most energetic g-ray selected pulsar. J1813 rotates as fast as the Crab and its Erot is similar to that of Vela, thus we expect the pulsar to be embedded in a bright PWN. Among RQ pulsars, J1813 shows the highest X-ray flux but no deep X-ray observations have ever been performed on this target. Exploiting both XMM and Chandra capabilities we ll be able to (i) discriminate J1813 from its pulsar wind nebula (ii) study its X-ray timing behaviour (iii) obtain accurate phase-averaged and phase-resolved spectra (iv) constrain the source distance.

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