Overview of the advanced x-ray imaging satellite (AXIS)

Reynolds, Christopher; Kara, Erin; Mushotzky, Richard F.; Ptak, Andrew; Koss, Michael J.; Williams, Brian J.; Allen, Steven W.; Bauer, Franz E.; Bautz, Marshall; Bogadhee, Arash; Burdge, Kevin B.; Cappelluti, Nico; Cenko, Brad; Chartas, George; Chan, Kai-Wing; Corrales, Lia; Daylan, Tansu; Falcone, Abe D.; Foord, Adi; Grant, Catherine E.; Habouzit, Melanie; Haggard, Daryl; Herrmann, Sven; Hodges-Kluck, Edmund; Kargaltsev, Oleg; King, George W.; Kounkel, Marina; Lopez, Laura A.; Marchesi, Stefano; McDonald, Michael; Meyer, Eileen; Miller, Eric D.; Nynka, Melania; Okajima, Takashi; Pacucci, Fabio; Russell, Helen R.; Safi-Harb, Samar; Strassun, Keivan G.; Trindade Falcão, Anna; Walker, Stephen A.; Wilms, Joern; Yukita, Mihoko; Zhang, William

doi:10.1117/12.2677468

Cited by 22 publications

(6 citation statements)

References 65 publications

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“…It will provide images with 1 ′′ − 2 ′′ resolution, across a 24 ′ diameter field-of-view, and sensitivity ten times greater than that of the Chandra X-ray Observatory. These advanced capabilities will complement the James Webb Space Telescope (JWST) and upcoming ground-and space-based observatories, positioning AXIS as a key instrument for future X-ray studies (see [106] for more details). In particular, the AXIS point spread function (PSF), field of view (FOV), and effective area (A e f f ) are expected to significantly strengthen our understanding of the X-ray activity of AGN pairs in ongoing mergers.…”

Section: The Power Of Axis For Agn Pair Studiesmentioning

confidence: 99%

“…AXIS plans to follow a "Wedding cake" strategy to perform its extragalactic surveys: (1) a deep 7 Ms observation of a single AXIS pointing (∼0.16 deg 2 , or ∼24 × 24 square arcmin); and (2) an intermediate-area (2.5 deg 2 ) and intermediate-depth (375 ks exposure per pointing) one. An AXIS serendipitous field built via combining Guest Observer observations (assuming 20 Ms of guaranteed non-galactic plane time, with a median of 50 ks per pointing) could cover 50 deg 2 with a sensitivity ∼10 −16 erg s −1 cm −2 (see [106] for more details on the surveys).…”

Section: Observations Of Dual Agns Via the Axis Agn Surveysmentioning

confidence: 99%

“…Thus, identifying this type of binary signature in blind searches is feasible with the large number of AGNs after combining the dedicated AXIS surveys and serendipitous observations. The depth in the latter, serendipitous field will reach ∼10 −16 erg s −1 cm −2 in an ∼50 deg 2 sky area [106], thus potentially yielding a large number of SMBHBs that display that signature.…”

Section: Spectral Hardening and Double Broad Fe Linesmentioning

confidence: 99%

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Tracking Supermassive Black Hole Mergers from kpc to sub-pc Scales with AXIS

Foord,

Cappelluti,

Liu

et al. 2024

Universe

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We present an analysis showcasing how the Advanced X-ray Imaging Satellite (AXIS), a proposed NASA Probe-class mission, will significantly increase our understanding of supermassive black holes undergoing mergers—from kpc to sub-pc scales. In particular, the AXIS point spread function, field of view, and effective area are expected to result in (1) the detection of hundreds to thousands of new dual AGNs across the redshift range 0<z<5 and (2) blind searches for binary AGNs that are exhibiting merger signatures in their light curves and spectra. AXIS will detect some of the highest-redshift dual AGNs to date, over a large range of physical separations. The large sample of AGN pairs detected by AXIS (over a magnitude more than currently known) will result in the first X-ray study that quantifies the frequency of dual AGNs as a function of redshift up to z=4.

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Section: The Power Of Axis For Agn Pair Studiesmentioning

confidence: 99%

Section: Observations Of Dual Agns Via the Axis Agn Surveysmentioning

confidence: 99%

Section: Spectral Hardening and Double Broad Fe Linesmentioning

confidence: 99%

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Tracking Supermassive Black Hole Mergers from kpc to sub-pc Scales with AXIS

Foord,

Cappelluti,

Liu

et al. 2024

Universe

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“…This will be especially useful in characterizations in the low energy response of instruments (<1 keV), where much astrophysical discovery space resides. 28,29 In the next sections, we give a brief description of our experimental setup, the technical details of the RNDR technique, and our experimental results. A summary and discussion of future plans can be found in Sec.…”

Section: Introductionmentioning

confidence: 99%

Demonstrating repetitive non-destructive readout with SiSeRO devices

Chattopadhyay,

Herrmann,

Orel

et al. 2024

J. Astron. Telesc. Instrum. Syst.

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We demonstrate so-called repetitive non-destructive readout (RNDR) for the first time on a single electron sensitive readout (SiSeRO) device. SiSeRO is a novel on-chip charge detector output stage for charge-coupled device image sensors, developed at MIT Lincoln Laboratory. This technology uses a p-MOSFET transistor with a depleted internal gate beneath the transistor channel. The transistor sourcedrain current is modulated by the transfer of charge into the internal gate. RNDR was realized by transferring the signal charge non-destructively between the internal gate and the summing well (SW), which is the last serial register. The advantage of the non-destructive charge transfer is that the signal charge for each pixel can be measured at the end of each transfer cycle, and by averaging for a large number of measurements (N cycle ), the total noise can be reduced by a factor of 1∕ ffiffiffiffiffiffiffiffiffiffiffiffi N cycle p . In our experiments with a prototype SiSeRO device, we implemented nine (N cycle ¼ 9) RNDR cycles, achieving around two electron readout noise (equivalent noise charge or ENC) with a spectral resolution close to the fano limit for silicon at 5.9 keV. These first results are extremely encouraging, demonstrating successful implementation of the RNDR technique in SiSeROs. They also lay the foundation for future experiments with more optimized test stands (better temperature control, larger number of RNDR cycles, and RNDR-optimized SiSeRO devices), which should be capable of achieving sub-electron noise sensitivities. This new device class presents an exciting technology for next generation astronomical X-ray telescopes requiring very low-noise spectroscopic imagers. The sub-electron sensitivity also adds the capability to conduct in-situ absolute calibration, enabling unprecedented characterization of the low energy instrument response.

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“…With a proposed on-axis angular resolution of 1.5 ′′ and an averaged PSF Half Energy Width (HEW) of 1.6 ′′ , coupled with an effective area of 4200 cm 2 at 1 keV, 830 cm 2 at 6 keV, and a 24 ′ diameter active field of view (i.e., ∼0.13 deg 2 ), AXIS [17] is poised to be a cutting-edge "X-ray survey machine" for the next decade. Benefitting from the low background provided by its low Earth orbit, AXIS will surpass Chandra by achieving depths that are one order of magnitude greater over a high-angular-resolution area that is at least 10 times larger.…”

Section: Introductionmentioning

confidence: 99%

Surveying the Onset and Evolution of Supermassive Black Holes at High-z with AXIS

Cappelluti,

Foord,

Marchesi

et al. 2024

Universe

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The nature and origin of supermassive black holes (SMBHs) remain an open matter of debate within the scientific community. While various theoretical scenarios have been proposed, each with specific observational signatures, the lack of sufficiently sensitive X-ray observations hinders the progress of observational tests. In this white paper, we present how AXIS will contribute to solving this issue. With an angular resolution of 1.5′′ on-axis and minimal off-axis degradation, we designed a deep survey capable of reaching flux limits in the [0.5–2] keV range of approximately 2 × 10−18 erg s−1 cm−2 over an area of 0.13 deg2 in approximately 7 million seconds (7 Ms). Furthermore, we planned an intermediate depth survey covering approximately 2 deg2 and reaching flux limits of about 2 × 10−17 erg s−1 cm−2 in order to detect a significant number of SMBHs with X-ray luminosities (LX) of approximately 1042 erg s−1 up to z ∼ 10. These observations will enable AXIS to detect SMBHs with masses smaller than 105 M⊙, assuming Eddington-limited accretion and a typical bolometric correction for Type II AGN. AXIS will provide valuable information on the seeding and population synthesis models of SMBHs, allowing for more accurate constraints on their initial mass function (IMF) and accretion history from z∼0–10. To accomplish this, AXIS will leverage the unique synergy of survey telescopes such as the JWST, Roman, Euclid, Vera Rubin Telescope, and the new generation of 30 m class telescopes. These instruments will provide optical identification and redshift measurements, while AXIS will discover the smoking gun of nuclear activity, particularly in the case of highly obscured AGN or peculiar UV spectra as predicted and recently observed by the JWST in the early Universe.

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Overview of the advanced x-ray imaging satellite (AXIS)

Cited by 22 publications

References 65 publications

Tracking Supermassive Black Hole Mergers from kpc to sub-pc Scales with AXIS

Tracking Supermassive Black Hole Mergers from kpc to sub-pc Scales with AXIS

Demonstrating repetitive non-destructive readout with SiSeRO devices

Surveying the Onset and Evolution of Supermassive Black Holes at High-z with AXIS

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