Detection of Galactic and Extragalactic Millimeter-wavelength Transient Sources with SPT-3G

Guns, S.; Foster, A.; Daley, C.; Rahlin, A.; Whitehorn, N.; Ade, Peter A. R.; Ahmed, Zeeshan; Anderes, Ethan; Anderson, A. J.; Archipley, Melanie; Avva, J. S.; Aylor, K.; Balkenhol, L.; Barry, P. S.; Thakur, R. Basu; Benabed, K.; Bender, A. N.; Benson, B. A.; Bianchini, F.; Bleem, L. E.; Bouchet, F. R.; Bryant, Lincoln; Byrum, K.; Carlstrom, J. E.; Carter, F. W.; Cecil, T. W.; Chang, C. L.; Chaubal, P.; Chen, G.; Cho, H. M.; Chou, T-L.; Cliche, J. F.; Crawford, T. M.; Cukierman, A.; Haan, T. de; Denison, Edward V.; Dibert, K.; Ding, J.; Dobbs, M.; Dutcher, D.; Everett, W.; Feng, Chang; Ferguson, K. R.; Fu, Jianyang; Galli, S.; Gambrel, A. E.; Gardner, R. W.; Goeckner-Wald, N.; Gualtieri, R.; Gupta, N.; Guyser, R.; Halverson, N. W.; Harke-Hosemann, A. H.; Harrington, N. L.; Henning, J. W.; Hilton, G. C.; Hivon, E.; Holder, G. P.; Holzapfel, W. L.; Hood, J. C.; Howe, D.; Huang, N.; Irwin, K. D.; Jeong, O. B.; Jonas, M.; Jones, Andrew; Khaire, T. S.; Knox, L.; Kofman, A. M.; Korman, M.; Kubik, D. L.; Kuhlmann, S.; Kuo, C.-L.; Lee, A. T.; Leitch, E. M.; Lowitz, A. E.; Lu, C.; Marrone, Dan; Meyer, S. S.; Michalik, D.; Millea, M.; Montgomery, J.; Nadolski, A.; Natoli, T.; Nguyen, H. T.; Noble, G. I.; Novosad, V.; Omori, Y.; Padin, S.; Pan, Z.; Paschos, Pascal; Pearson, John E.; Phadke, Kedar A.; Posada, C. M.; Prabhu, K.; Quan, Wei; Reichardt, C. L.; Riebel, D.; Riedel, Benedikt; Rouble, M.; Ruhl, J. E.; Sayre, J. T.; Schiappucci, E.; Shirokoff, E.; Smecher, G.; Sobrin, J. A.; Stark, A. A.; Stephen, J.; Story, K. T.; Suzuki, Aritoki; Thompson, K. L.; Thorne, Ben; Tucker, C.; Umiltà, Caterina; Vale, L. R.; Vieira, J. D.; Wang, G.; Wu, W. L. K.; Yefremenko, V.; Yoon, K. W.; Young, M. R.; Zhang, L.

doi:10.3847/1538-4357/ac06a3

Cited by 25 publications

(33 citation statements)

References 37 publications

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“…Until recently, there was only one untargeted transient survey specific to the millimeter band (Whitehorn et al 2016). Within the past year, the Atacama Cosmology Telescope (ACT; Thornton et al 2016) and the South Pole Telescope (SPT; Carlstrom et al 2011) published blind discoveries of bright (millijansky) transients (Naess et al 2021;Guns et al 2021), including several of extragalactic origin (Guns et al 2021). The 100 GHz lightcurve of AT 2020xnd (Figure 2) is the most luminous ever obtained for a nonrelativistic cosmic explosion, and in this section, we estimate the rate of such events in present and future millimeter transient surveys, summarized in Table 4.…”

Section: Rates In Millimeter Surveysmentioning

confidence: 99%

Luminous Millimeter, Radio, and X-Ray Emission from ZTF 20acigmel (AT 2020xnd)

Margalit

Bremer

et al. 2022

ApJ

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Observations of the extragalactic (z = 0.0141) transient AT 2018cow established a new class of energetic explosions shocking a dense medium, producing luminous emission at millimeter and submillimeter wavelengths. Here we present detailed millimeter- through centimeter-wave observations of a similar transient, ZTF 20acigmel (AT 2020xnd), at z = 0.2433. Using observations from the NOrthern Extended Millimeter Array and the Very Large Array, we model the unusual millimeter and radio emission from AT 2020xnd under several different assumptions and ultimately favor synchrotron radiation from a thermal electron population (relativistic Maxwellian). The thermal electron model implies a fast but subrelativistic (v ≈ 0.3c) shock and a high ambient density (n e ≈ 4 × 103 cm−3) at Δt ≈ 40 days. The X-ray luminosity of L X ≈ 1043 erg s−1 exceeds simple predictions from the radio and UVOIR luminosity and likely has a separate physical origin, such as a central engine. Using the fact that month-long luminous (L ν ≈ 2 × 1030 erg s−1 Hz−1 at 100 GHz) millimeter emission appears to be a generic feature of transients with fast (t 1/2 ≈ 3 days) and luminous (M peak ≈ −21 mag) optical light curves, we estimate the rate at which transients like AT 2018cow and AT 2020xnd will be detected by future wide-field millimeter transient surveys such as CMB-S4 and conclude that energetic explosions in dense environments may represent a significant population of extragalactic transients in the 100 GHz sky.

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Section: Rates In Millimeter Surveysmentioning

confidence: 99%

Luminous Millimeter, Radio, and X-Ray Emission from ZTF 20acigmel (AT 2020xnd)

Margalit

Bremer

et al. 2022

ApJ

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“…The LAT will be able to make precise measurements of the small-scale temperature and polarization power spectra, as well as the CMB lensing spectrum (The Simons Observatory Collaboration 2019). Additionally, the LAT will detect tens of thousands of clusters using the thermal SZ effect, as well as numerous extragalactic sources and transient microwave objects (Naess et al 2021;Guns et al 2021). There are even prospects for the LAT to detect Oort clouds around nearby stars (Blake et al 2019;Orlowski-Scherer et al 2019) or additional planets in our solar system (Baxter et al 2018).…”

Section: Introductionmentioning

confidence: 99%

The Simons Observatory Large Aperture Telescope Receiver

Zhu

Bhandarkar

Coppi

et al. 2021

ApJS

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The Simons Observatory is a ground-based cosmic microwave background experiment that consists of three 0.4 m small-aperture telescopes and one 6 m Large Aperture Telescope, located at an elevation of 5300 m on Cerro Toco in Chile. The Simons Observatory Large Aperture Telescope Receiver (LATR) is the cryogenic camera that will be coupled to the Large Aperture Telescope. The resulting instrument will produce arcminute-resolution millimeter-wave maps of half the sky with unprecedented precision. The LATR is the largest cryogenic millimeter-wave camera built to date, with a diameter of 2.4 m and a length of 2.6 m. The coldest stage of the camera is cooled to 100 mK, the operating temperature of the bolometric detectors with bands centered around 27, 39, 93, 145, 225, and 280 GHz. Ultimately, the LATR will accommodate 13 40 cm diameter optics tubes, each with three detector wafers and a total of 62,000 detectors. The LATR design must simultaneously maintain the optical alignment of the system, control stray light, provide cryogenic isolation, limit thermal gradients, and minimize the time to cool the system from room temperature to 100 mK. The interplay between these competing factors poses unique challenges. We discuss the trade studies involved with the design, the final optimization, the construction, and ultimate performance of the system.

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“…Finally, both ACT and SPT have revealed dramatic time variability in the microwave sky and thus a vast discovery space for next-generation CMB experiments (Guns et al 2021;Naess et al 2021b). Microwave transient science is an active area of development within SO, but as it lies outside the scope of the science cases and forecasts presented here, a detailed exploration is left for future work.…”

Section: Discussionmentioning

confidence: 97%

The Simons Observatory: Galactic Science Goals and Forecasts

Hensley

Clark

Fanfani

et al. 2022

ApJ

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Observing in six frequency bands from 27 to 280 GHz over a large sky area, the Simons Observatory (SO) is poised to address many questions in Galactic astrophysics in addition to its principal cosmological goals. In this work, we provide quantitative forecasts on astrophysical parameters of interest for a range of Galactic science cases. We find that SO can: constrain the frequency spectrum of polarized dust emission at a level of Δβ d ≲ 0.01 and thus test models of dust composition that predict that β d in polarization differs from that measured in total intensity; measure the correlation coefficient between polarized dust and synchrotron emission with a factor of two greater precision than current constraints; exclude the nonexistence of exo-Oort clouds at roughly 2.9σ if the true fraction is similar to the detection rate of giant planets; map more than 850 molecular clouds with at least 50 independent polarization measurements at 1 pc resolution; detect or place upper limits on the polarization fractions of CO(2–1) emission and anomalous microwave emission at the 0.1% level in select regions; and measure the correlation coefficient between optical starlight polarization and microwave polarized dust emission in 1° patches for all lines of sight with N H ≳ 2 × 1020 cm−2. The goals and forecasts outlined here provide a roadmap for other microwave polarization experiments to expand their scientific scope via Milky Way astrophysics. 37 37 A supplement describing author contributions to this paper can be found at https://simonsobservatory.org/wp-content/uploads/2022/02/SO_GS_Contributions.pdf.

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Detection of Galactic and Extragalactic Millimeter-wavelength Transient Sources with SPT-3G

Cited by 25 publications

References 37 publications

Luminous Millimeter, Radio, and X-Ray Emission from ZTF 20acigmel (AT 2020xnd)

Luminous Millimeter, Radio, and X-Ray Emission from ZTF 20acigmel (AT 2020xnd)

The Simons Observatory Large Aperture Telescope Receiver

The Simons Observatory: Galactic Science Goals and Forecasts

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