Advanced CCD imaging spectrometer (ACIS) instrument on the Chandra X-ray Observatory

Garmire, G. P.; Bautz, M. W.; Ford, P. G.; Nousek, J. A.; Ricker, G.

doi:10.1117/12.461599

Cited by 699 publications

(247 citation statements)

References 25 publications

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“…During the two long Chandra/Advanced CCD Imaging Spectrometer (ACIS; Garmire et al 2003) observations performed in 2011 the source was located in one of the two ACIS-I, frontilluminated CCDs, operated in full-imaging timed-exposure mode (no gratings) and with a frame time of 3.24 s. New level 2 event files were generated with the Chandra Interactive Analysis of Observations (CIAO) software version 4.8, and products extracted adopting standard procedures. We refer the reader to Israel et al (2016) for additional details on the data reduction not contained in this paper.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

AX J1910.7+0917: the slowest X-ray pulsar

Sidoli

Israel

Esposito

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Pulsations from the high mass X-ray binary AX J1910.7+0917 were discovered during Chandra observations performed in 2011 (Israel et al. 2016). We report here more details on this discovery and discuss the source nature. The period of the X-ray signal is P = 36200 ± 110 s, with a pulsed fraction, P F , of 63±4%. Given the association with a massive B-type companion star, we ascribe this long periodicity to the rotation of the neutron star, making AX J1910.7+0917 the slowest known X-ray pulsar. We report also on the spectroscopy of XMM-Newton observations that serendipitously covered the source field, resulting in an highly absorbed (column density almost reaching 10 23 cm −2 ), power law X-ray spectrum. The Xray flux is variable on a timescale of years, spanning a dynamic range 60. The very long neutron star spin period can be explained within a quasi-spherical settling accretion model, that applies to low luminosity, wind-fed, X-ray pulsars.

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Section: Observations and Data Reductionmentioning

confidence: 99%

AX J1910.7+0917: the slowest X-ray pulsar

Sidoli

Israel

Esposito

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…A Chandra (Weisskopf et al 2000) ACIS-S (Garmire et al 2003) observation of NGC 6286 was carried out on UT 2009 September 18 (PI: Swartz) with an exposure of 14.2 ks. The data reduction was performed following the standard procedure using CIAO v.4.6.…”

Section: Chandramentioning

confidence: 99%

NuSTAR UNVEILS A HEAVILY OBSCURED LOW-LUMINOSITY ACTIVE GALACTIC NUCLEUS IN THE LUMINOUS INFRARED GALAXY NGC 6286

Ricci

Bauer

Treister

et al. 2016

ApJ

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We report the detection of a heavily obscured active galactic nucleus (AGN) in the luminous infrared galaxy (LIRG) NGC 6286 identified in a 17.5 ks Nuclear Spectroscopic Telescope Array observation. The source is in an early merging stage and was targeted as part of our ongoing NuSTAR campaign observing local luminous and ultraluminous infrared galaxies in different merger stages. NGC 6286 is clearly detected above 10 keV and by including the quasi-simultaneous Swift/XRT and archival XMM-Newton and Chandra data, we find that the source is heavily obscured (N H ;(0.95−1.32) × 10 24 cm −2 ) with a column density consistent with being Compton-thick (CT, N log cm 24The AGN in NGC 6286 has a low absorption-corrected luminosity (L 2−10 keV ∼ 3 −20 × 10 41 erg s −1 ) and contributes 1% to the energetics of the system. Because of its low luminosity, previous observations carried out in the soft X-ray band (<10 keV) and in the infrared did not notice the presence of a buried AGN. NGC 6286 has multiwavelength characteristics typical of objects with the same infrared luminosity and in the same merger stage, which might imply that there is a significant population of obscured low-luminosity AGNs in LIRGs that can only be detected by sensitive hard X-ray observations.

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“…To search for the diskless stellar population predicted by PW10 and hence improve our understanding of the star formation history in M17 SWex, we observed G14.225-0.506 using the Advanced CCD Imaging Spectrometer (ACIS; Garmire et al 2003) of the Chandra X-ray Observatory. This observation was designed to be combined with near-and mid-IR photometry from the Spitzer Space Telescope Galactic Legacy IR Mid-Plane Survey Extraordinaire (GLIMPSE; Benjamin et al 2003;Churchwell et al 2009) and MIPSGAL Galactic plane survey (Carey et al 2009), 2MASS, and the UKIDSS Galactic Plane Survey (Lawrence et al 2007;Lucas et al 2008).…”

Section: Introductionmentioning

confidence: 99%

“…We discuss the G014.33-00.64 region in more detail in Section 5.5. (Garmire et al 2003). The point source catalog and analysis presented in this work are restricted to ACIS-I, because the angular resolution of the Chandra grazingincidence mirrors is poor at the large off-axis angles (q > ¢ 9 ) of the ACIS-S detectors, and the ACIS-S detectors covered a part of the sky far from the M17 SWex IRDC filaments.…”

Section: Introductionmentioning

confidence: 99%

RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

Povich

Townsley

Robitaille

et al. 2016

ApJ

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We present a catalog of 840 X-ray sources and first results from a 100 ks Chandra X-ray Observatory imaging study of the filamentary infrared (IR) dark cloud G014.225-00.506, which forms the central regions of a larger cloud complex known as the M17 southwest extension (M17 SWex). In addition to the rich population of protostars and young stellar objects with dusty circumstellar disks revealed by archival data from the Spitzer Space Telescope, we discover a population of X-ray-emitting, intermediate-mass pre-main-sequence stars that lack IR excess emission from circumstellar disks. We model the IR spectral energy distributions of this source population to measure its mass function and place new constraints on the destruction timescales for the inner dust disk for 2-8 M ☉ stars. We also place a lower limit on the star formation rate (SFR) and find that it is quite high (  M 0.007 M ☉ yr −1 ), equivalent to several Orion Nebula Clusters in G14.225-0.506 alone, and likely accelerating. The cloud complex has not produced a population of massive, O-type stars commensurate with its SFR. This absence of very massive (20 M ☉ ) stars suggests that either (1) M17 SWex is an example of a distributed mode of star formation that will produce a large OB association dominated by intermediate-mass stars but relatively few massive clusters, or (2) the massive cores are still in the process of accreting sufficient mass to form massive clusters hosting O stars.

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Advanced CCD imaging spectrometer (ACIS) instrument on the Chandra X-ray Observatory

Cited by 699 publications

References 25 publications

AX J1910.7+0917: the slowest X-ray pulsar

AX J1910.7+0917: the slowest X-ray pulsar

NuSTAR UNVEILS A HEAVILY OBSCURED LOW-LUMINOSITY ACTIVE GALACTIC NUCLEUS IN THE LUMINOUS INFRARED GALAXY NGC 6286

RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

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