SOFIA-HIRMES: Looking Forward to the HIgh-Resolution Mid-infrarEd Spectrometer

Richards, Samuel N.; Moseley, S. H.; Stacey, G. J.; Greenhouse, Matthew A.; Kutyrev, A.; Arendt, Richard G.; Atanasoff, Hristo; Banks, S.; Brekosky, Regis P.; Brown, Arthur; Bulcha, Berhanu; Cazeau, Tony; Choi, Michael K.; Colazo, Felipe; Engler, Chuck; Hadjimichael, Theodore; Hays-Wehle, J. P.; Henderson, C.; Hsieh, Wen‐Ting; Huang, Jeffrey; Jenstrom, Iver; Kellogg, Jim; Kimball, Mark O.; Kovács, A.; Leiter, Steve; Maher, Steve; McMurray, Robert E.; Melnick, Gary J.; Mentzell, Eric; Mikula, Vilem; Miller, Timothy M.; Nagler, Peter C.; Nikola, Thomas; Oxborrow, Joseph; Pontoppidan, K. M.; Rangwala, Naseem; Rhodes, Alan; Roberge, Aki; Rosner, S. J.; Rostem, Karwan; Rustemeyer, Nancy; Sharp, Elmer H.; Sparr, Leroy; Stevanović, Dejan; Taraschi, Peter; Temi, P.; Vacca, William D.; Lorenzo, Jordi Vila Hernandez de; Wohler, Bill; Wollack, Edward J.; Wilks, Shannon

doi:10.1142/s2251171718400159

Cited by 10 publications

(3 citation statements)

References 18 publications

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“…The HIRMES instrument was proposed to be added to the SOFIA observatory, offering a spectral resolution of 3 km s −1 at 112 μm. If built and deployed, HIRMES was projected to have a sensitivity similar to PACS (Richards et al 2018) and could perform deep surveys for HD emission, opening up the ability to provide a robust diagnostic of gas mass. The planned spectral resolution on HIRMES is enough to fully resolve the HD emission line for inclined disks, which will provide unique constraints on the radial distribution of disk gas.…”

Section: Future Hd Observationsmentioning

confidence: 99%

The TW Hya Rosetta Stone Project. III. Resolving the Gaseous Thermal Profile of the Disk

Calahan¹,

Bergin²,

Zhang³

et al. 2021

ApJ

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The thermal structure of protoplanetary disks is a fundamental characteristic of the system that has wide-reaching effects on disk evolution and planet formation. In this study, we constrain the 2D thermal structure of the protoplanetary disk TW Hya structure utilizing images of seven CO lines. This includes new ALMA observations of 12 CO J = 2-1 and C 18 O J = 2-1 as well as archival ALMA observations of 12 CO J = 3-2, 13 CO J = 3-2 and 6-5, and C 18 O J = 3-2 and 6-5. Additionally, we reproduce a Herschel observation of the HD J = 1-0 line flux and the spectral energy distribution and utilize a recent quantification of CO radial depletion in TW Hya. These observations were modeled using the thermochemical code RAC2D, and our best-fit model reproduces all spatially resolved CO surface brightness profiles. The resulting thermal profile finds a disk mass of 0.025 M e and a thin upper layer of gas depleted of small dust with a thickness of ∼1.2% of the corresponding radius. Using our final thermal structure, we find that CO alone is not a viable mass tracer, as its abundance is degenerate with the total H 2 surface density. Different mass models can readily match the spatially resolved CO line profiles with disparate abundance assumptions. Mass determination requires additional knowledge, and, in this work, HD provides the additional constraint to derive the gas mass and support the inference of CO depletion in the TW Hya disk. Our final thermal structure confirms the use of HD as a powerful probe of protoplanetary disk mass. Additionally, the method laid out in this paper is an employable strategy for extraction of disk temperatures and masses in the future.

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Section: Future Hd Observationsmentioning

confidence: 99%

The TW Hya Rosetta Stone Project. III. Resolving the Gaseous Thermal Profile of the Disk

Calahan¹,

Bergin²,

Zhang³

et al. 2021

ApJ

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“…Stratospheric Observatory for Infra-red Astrophysics (SOFIA). HIRMES was designed to probe several important aspects of protoplanetary formation by providing low (∼600) to very high (∼100000) spectroscopy in the 25-122 micron spectral regime [1].…”

Section: Please Provide Feedbackmentioning

confidence: 99%

Excess Heat Capacity in Mo/Au Transition Edge Sensor Bolometric Detectors

Brown

Brekosky

Colazo-Petit³

et al. 2021

IEEE Trans. Appl. Supercond.

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Excess heat capacity in a bolometric detector has the consequence of increasing or leading to multiple device time constants. The Mo/Au bilayer transition edge sensor (TES) bolometric detectors initially fabricated for the high resolution mid-infrared spectrometer (HIRMES) exhibited two response thermalization scales, one of which is a few times longer than estimates based upon the properties of the bulk materials employed in the design. The relative contribution of this settling time to the overall time response of the detectors is roughly proportional to the pixel area, which ranges between ∼0.3 and 2.6 mm 2 . Use of laser ablation to remove sections of the silicon membranes comprising the pixels results in a detector response with a smaller contribution from the secondary time constant. Additional information about the nature of this excess heat capacity is gleaned from glancing incidence X-ray diffraction, which reveals the presence of molybdenum silicides near the silicon surface which is a consequence of the bi-layer deposition. Quantitative analysis of the concentration of excess molybdenum, estimated with secondary ion mass spectroscopy, is commensurate to the additional heat capacity needed to explain the anomalous time response of the detectors.

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“…We begin by mentioning the High Resolution Mid-InfrarEd Spectrometer (HIRMES) which has been developed by NASA Goddard for the Stratospheric Observatory for Infrared Astronomy (SOFIA). HIRMES is optimized to detect neutral atomic oxygen, water, as well as normal and deuterated hydrogen between 28 and 112µm (Richards et al, 2018). A primarily scientific goal is to investigate the molecular and atomic gas content of protoplanetary disks as well as their ice features, e.g.…”

Section: Future Observational Prospectsmentioning

confidence: 99%

Jets from Young Stars

Ray,

Ferreira

2020

Preprint

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Jets are ubiquitous in the Universe and, as demonstrated by this volume, are seen from a large number of astrophysical objects including active galactic nuclei, gamma ray bursters, micro-quasars, proto-planetary nebulae, young stars and even brown dwarfs. In every case they seem to be accompanied by an accretion disk and, while the detailed physics may change, it has been suggested that the same basic mechanism is responsible for generating the jet. Although we do not understand what that mechanism is, or even if it is universal, it is thought to involve the centrifugal ejection of matter from the disk along magnetic field lines. For a number of reasons, in particular their proximity and the abundant range of diagnostics to determine their characteristics, jets from young stars and their associated outflows may offer us the best opportunity to discover how jets are generated and the nature of the link between outflows and their accretion disks. Recently it has become clear that jets may be fundamental to the star formation process in removing angular momentum from the surrounding protoplanetary disk thereby allowing accretion to proceed. Moreover, with the realisation that planetary formation begins much earlier than previously thought, jets may also help forge planets by determining initial environmental characteristics. This seems to be particularly true within the so-called terrestrial planet forming zone. Here we review observations of jets from young stars which have greatly benefitted from new facilities such as ALMA, space observatories * To appear in the New Astronomy Reviews special volume 100 Years of Jets (eds. Rob Fender and Ralph Wijers)

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SOFIA-HIRMES: Looking Forward to the HIgh-Resolution Mid-infrarEd Spectrometer

Cited by 10 publications

References 18 publications

The TW Hya Rosetta Stone Project. III. Resolving the Gaseous Thermal Profile of the Disk

The TW Hya Rosetta Stone Project. III. Resolving the Gaseous Thermal Profile of the Disk

Excess Heat Capacity in Mo/Au Transition Edge Sensor Bolometric Detectors

Jets from Young Stars

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