After our report on the flux decay of the neutron star transient SAX J1750.8-2900 (ATel #1662) we have continued monitoring the source with Swift-XRT in order to study its transition to quiescence. In these observations (performed between August 14th. and October 8th.) we detect the source at different flux levels, with the corresponding luminosity

Swift J1357.2-0933 is a confirmed very faint black hole X-ray transient and has a short estimated orbital period of 2.8 h. We observed Swift J1357.2-0933 for ˜50 ks with XMM-Newton in 2013 July during its quiescent state. The source is clearly detected at a 0.5-10 keV unabsorbed flux of ˜3 × 10-15 erg cm-2 s-1. If the source is located at a

The black hole (BH) binary V404 Cyg entered the outburst phase in 2015 June after 26 yr of X-ray quiescence, and with its behaviour broke the outburst evolution pattern typical of most BH binaries. We observed the entire outburst with the Swift satellite and performed time-resolved spectroscopy of its most active phase, obtaining over a thousand

IBIS-ISGRI observations on 2010-10-10 (Bordas et al. ATel #2919) as well as RXTE-PCA scans on 2010-10-09 (http://lheawww.gsfc.nasa.gov/users/craigm/galscan/html/EXO_1745-248.html) showed enhanced X-ray emission from the direction of the globular cluster Terzan 5. We analysed a ~500 s Swift-XRT observation of the field starting on 2010-10-10 01:32

We report a Swift follow-up observation of the very faint X-ray transient source XTE J1728-295 (also IGR J17285-2922, ATel #2825) currently in the decaying phase of its recent outburst (ATel #2823, #2824, #2869). The observation was performed on 2010-10-29 07:07:35 UTC for a duration of 2 ks, and was observed in Photon Counting (PC) mode

Spectropolarimetric observations in photospheric lines reveal a wealth of information on physical parameters of the solar atmosphere like magnetic field strength and di rection or the line-of sight velocity. These observations require the measurement of the four Stokes parameters at a sample of N wavelength positions around the core of the spectral