NuSTAR: NASA-ның рентгендік телескопы және зерттеулері

NASA X ray space telescope of the Explorer program

NuSTAR is the eleventh mission of NASA's Small Explorer (SMEX 11) satellite program and the first space based direct imaging X ray telescope at energies beyond those of the Chandra X ray Observatory and XMM Newton. It was successfully launched on 13 June 2012, having previously been delayed from 21 March 2012 due to software issues with the launch vehicle. The mission's primary scientific goals are to conduct a deep survey for black holes a billion times more massive than the Sun, to investigate how particles are accelerated to very high energy in active galaxies, and to understand how the elements are created in the explosions of massive stars by imaging supernova remnants. Having completed a two year primary mission, NuSTAR is in its year of operation.

NuSTAR's predecessor, the High Energy Focusing Telescope (HEFT), was a balloon borne version that carried telescopes and detectors constructed using similar technologies. In February 2003, NASA issued an Explorer program Announcement of Opportunity (AoO). In response, NuSTAR was submitted to NASA in May 2003, as one of 36 mission proposals vying to be the tenth and eleventh Small Explorer missions. The program was cancelled in February 2006 as a result of cuts to science in NASA's 2007 budget. On 21 September 2007, it was announced that the program had been restarted, with an expected launch in August 2011, though this was later delayed to June 2012. The principal investigator is Fiona A. Harrison of the California Institute of Technology (Caltech). Other major partners include the Jet Propulsion Laboratory (JPL), University of California, Berkeley, Technical University of Denmark (DTU), Columbia University, Goddard Space Flight Center (GSFC), Stanford University, University of California, Santa Cruz, Sonoma State University, Lawrence Livermore National Laboratory, and the Italian Space Agency (ASI). NuSTAR's major industrial partners include Orbital Sciences Corporation and ATK Space Components.

NASA contracted with Orbital Sciences Corporation to launch NuSTAR (mass ) on a Pegasus XL launch vehicle on 21 March 2012. After a launch meeting on 15 March 2012, the launch was pushed further back to allow time to review flight software used by the launch vehicle's flight computer. The launch was conducted successfully at 16:00:37 UTC on 13 June 2012 The Pegasus launch vehicle was dropped from the L 1011 'Stargazer' aircraft. On 22 June 2012, it was confirmed that the mast was fully deployed.

Unlike visible light telescopes – which employ mirrors or lenses working with normal incidence – NuSTAR has to employ grazing incidence optics to be able to focus X rays. For this two conical approximation Wolter telescope design optics with focal length are held at the end of a long deployable mast. A laser metrology system is used to determine the exact relative positions of the optics and the focal plane at all times, so that each detected photon can be mapped back to the correct point on the sky even if the optics and the focal plane move relative to one another during an exposure. Each focusing optic consists of 133 concentric shells. One particular innovation enabling NuSTAR is that these shells are coated with depth graded multilayers (alternating atomically thin layers of a high density and low density material); with NuSTAR's choice of Pt/SiC and W/Si multilayers, this enables reflectivity up to 79 keV (the platinum K edge energy). The optics were produced, at Goddard Space Flight Center, by heating thin sheets of flexible glass in an oven so that they slumped over precision polished cylindrical quartz mandrels of the appropriate radius. The coatings were applied by a group at the Danish Technical University. The shells were then assembled, at the Nevis Laboratories of Columbia University, using graphite spacers machined to constrain the glass to the conical shape, and held together by epoxy. There are 4680 mirror segments in total (the 65 inner shells each comprise six segments and the 65 outer shells twelve; there are upper and lower segments to each shell, and there are two telescopes); there are five spacers per segment. Since the epoxy takes 24 hours to cure, one shell is assembled per day – it took four months to build up one optic. The actual telescope consists of two separate Focal Plane Modules (FPMs) labelled FPMA and FPMB. These two FPMs are built to be similar, though they are not identical. Depending on the source and on the observation, one of the modules will usually report higher counts. This is corrected for in the science results step, usually by apply a constant multiplier during spectral fitting and light curve analysis. The expected point spread function for the flight mirrors is 43 arcseconds, giving a spot size of about two millimeters at the focal plane; this is unprecedentedly good resolution for focusing hard X ray optics, though it is about one hundred times worse than the best resolution achieved at longer wavelengths by the Chandra X ray Observatory.

Each focusing optic has its own focal plane module, consisting of a solid state cadmium zinc telluride (CdZnTe) pixel detector surrounded by a cesium iodide (CsI) anti coincidence shield. One detector unit — or focal plane — comprises four (two by two) detectors, manufactured by eV Products. Each detector is a rectangular crystal of dimension and thickness ~ that have been gridded into pixels (each pixel subtending 12.3 arcseconds) and provides a total of 12 arcminutes field of view (FoV) for each focal plane module. The cadmium zinc telluride (CdZnTe) detectors are state of the art room temperature semiconductors that are very efficient at turning high energy photons into electrons. The electrons are digitally recorded using custom application specific integrated circuits (ASICs) designed by the NuSTAR California Institute of Technology (CalTech) Focal Plane Team. Each pixel has an independent discriminator and individual X ray interactions trigger the readout process. On board processors, one for each telescope, identify the row and column with the largest pulse height and read out pulse height information from this pixel as well as its eight neighbors. The event time is recorded to an accuracy of 2 μs relative to the on board clock. The event location, energy, and depth of interaction in the detector are computed from the nine pixel signals. The focal planes are shielded by cesium iodide (CsI) crystals that surround the detector housings. The crystal shields, grown by Saint Gobain, register high energy photons and cosmic rays which cross the focal plane from directions other than the along the NuSTAR optical axis. Such events are the primary background for NuSTAR and must be properly identified and subtracted in order to identify high energy photons from cosmic sources. The NuSTAR active shielding ensures that any CZT detector event coincident with an active shield event is ignored.

NuSTAR has demonstrated its versatility, opening the way to many new discoveries in a wide variety of areas of astrophysical research since its launch.

In February 2013, NASA revealed that NuSTAR, along with the XMM Newton space observatory, has measured the spin rate of the supermassive black hole at the center of the galaxy NGC 1365. By measuring the frequency change of X ray light emitted from the black hole corona, NuSTAR was able to view material from the corona be drawn closer to the event horizon. This caused inner portions of the black hole's accretion disk to be illuminated with X rays, allowing this elusive region to be studied by astronomers for spin rates. |image3=PIA18467 NuSTAR Plot BlackHole BlursLight 20140812. png|caption3=Blurring of X rays near black hole(NuSTAR; 12 August 2014)

In January 2017, researchers from Durham University and the University of Southampton, leading a coalition of agencies using NuSTAR data, announced the discovery of supermassive black holes at the center of nearby galaxies NGC 1448 and IC 3639.

In March 2nd of 2017, NuSTAR published an article to Nature detailing observations of wind temperature variations around AGN IRAS 13224−3809. By detecting periodic absences of absorption lines in the X ray spectrum from the accretion disk winds, NuSTAR and XMM Newton observed heating and cooling cycles of the relativistic winds leaving the accretion disk.

NuSTAR and XMM Newton detected X rays emitted behind the supermassive black hole within Seyfert 1 galaxy I Zwicky 1. Upon studying the flashes of light emitted by the corona of the black hole, researchers noticed that some detected light arrived to the detector later than the rest, with a corresponding change in frequency. The Stanford University team of scientists that led the study concluded that this change was directly attributable to radiation from the flash reflecting off of the accretion disk on the opposing side of the black hole. The path of this reflected light was bent by the high spacetime curvature, directed to the detector after the initial flash.

In April 6th of 2023, the NuSTAR team confirmed that neutron star M82 X 2 was emitting more radiation than was physically thought possible due to the Eddington limit, officially labeling it as an Ultraluminous X ray source (ULX).