Significance sky map around the region of PSR J2032+4127 / MT91. For details, see Figure 2 below.

Reference: A.U. Abeysekara et al. (The VERITAS and MAGIC Collaborations), ApJ Letters 867: L19, 2018

Full text version

ArXiv: ArXiV:1810.05271

Contacts: Ralph Bird

PSR J2032+4127 / MT91 213 is a 50 year period pulsar / Be star binary system that reached periastron in November 13, 2017.  It presented a unique opportunity to study what was potentially only the second gamma-ray binary where the type of the compact object is known.  In this paper we present the results of VERITAS and MAGIC observations of the system between 100 GeV and 20 TeV with observations spanning from 18 months prior to periastron to one month after periastron. A new, point-like, gamma-ray source was detected, coincident with the location of PSR J2032+4127 / MT91 213.  We present the gamma-ray light curve and spectrum which are well-characterized over the periastron passage. The flux was variable over at least an order of magnitude, peaking at periastron, thus providing a firm association of the TeV source with the pulsar / Be star system. Observations prior to periastron show a cutoff in the spectrum at an energy around 0.5 TeV. This result adds a new member to the small population of known TeV binaries, and it identifies only the second source of this class in which the nature and properties of the compact object are firmly established.  This system lies at the edge of the extended TeV source TeV J2032+4130, likely the pulsar wind nebula (PWN) associated with PSR J2032+4127; this makes this the first binary system where an associated PWN has been detected.

We compared the gamma-ray results with the light curve measured with the X-ray Telescope (XRT) on board the Neil Gehrels Swift Observatory and with the predictions of recent theoretical models of the system. We conclude that significant revision of the models is required to explain the details of the emission we have observed, and we discuss the relationship between the binary system and the overlapping steady extended source, TeV J2032+4130.


FITS files: Significance map (VERITAS); Significance map (MAGIC); VERITAS spectral points; MAGIC spectral points


Figures from paper (click to get full size image):


Figure 1:  Upper panels (left axes) show the 0.3-10.0 keV background-subtracted Swift-XRT energy-flux light curve (red circles) of PSR J2032+4127 / MT91 213. For clarity, observations with exposures less than 1.4 ks are excluded from the plot. Lower panels show the > 200 GeV photon-flux light curves from VERITAS (green triangles) and MAGIC (blue squares). The left plot shows the full light curve, while the right plot shows only the months around periastron. The horizontal solid lines indicate the average flux prior to 2017 for the respective experiments. The solid gray lines (right axes) are the energy-flux light curve predictions from Li et al. (2018) for X-rays and updated predictions from Takata et al. (2017) using the parameters from Li et al. (2018) (Takata, private communication) for VHE gamma rays. Both models assume an inclination angle of 60o . The vertical
gray dashed line indicates periastron.
Figure 2: Signi ficance sky maps of the region around PSR J2032+4127 / MT91 213 showing both the VERITAS (left) and MAGIC (right) results for observations during 2017 fall. The position of PSR J2032+4127 / MT91 213 is shown as a black "+", the centroid of the gamma-ray emission as a black "o ", the position and extension for the respective telescope's measurements of TeV J2032+4130 are shown as a black "X " and a dashed line, and the position of Cygnus X-3 is shown with a white diamond. The white circle in the lower left hand corner is of radius 0.1o , the approximate point spread function for these measurements at 1 TeV. The wobble positions are shown as white "X".

Figure 3: Spectral energy distributions for PSR J2032+4127 / MT91 213 and TeV J2032+4130 from VERITAS (left) and MAGIC (right). The blue butterflies are the spectral fi ts to TeV J2032+4130. The red butterflies in the upper plots are fits to the 2017 fall data: the sum of a power-law fi t to TeV J2032+4130 and a cutoff power-law fi t to PSR J2032+4127 / MT91 213. In the bottom plots, orange is the fi t to the low-state data (PSR J2032+4127 / MT91 213 is fit with a cutoff ) while green represents the high-state data (PSR J2032+4127 / MT91 213 is fi t with a power law). The fit parameters are given in Table 1 and the time periods are defi ned in the text.