Submillimeter Variability in the Envelope and Warped Protostellar Disk of the Class 0 Protostar HOPS 358
The James Clerk Maxwell Telescope (JCMT) Transient Survey recently discovered that the Class 0 protostar HOPS 358 decreased in 350 GHz continuum brightness by ∼25% over the course of 4 yr before brightening again for the next 4. The JCMT light curve can be fit by a long-timescale dip lasting roughly...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/adaf9b |
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| author | Patrick D. Sheehan Doug Johnstone Carlos Contreras Peña Seonjae Lee Gregory Herczeg Jeong-Eun Lee Steve Mairs John J. Tobin Hyeong-Sik Yun The JCMT Transient Team |
| author_facet | Patrick D. Sheehan Doug Johnstone Carlos Contreras Peña Seonjae Lee Gregory Herczeg Jeong-Eun Lee Steve Mairs John J. Tobin Hyeong-Sik Yun The JCMT Transient Team |
| author_sort | Patrick D. Sheehan |
| collection | DOAJ |
| description | The James Clerk Maxwell Telescope (JCMT) Transient Survey recently discovered that the Class 0 protostar HOPS 358 decreased in 350 GHz continuum brightness by ∼25% over the course of 4 yr before brightening again for the next 4. The JCMT light curve can be fit by a long-timescale dip lasting roughly 8 yr. A shorter-timescale periodicity is also apparent with a period of 1.75 yr and a small 3% amplitude. NEOWISE monitoring reveals that the mid-infrared wavelength brightness of HOPS 358 follows a similar long-term pattern in time. Here, we present a study of nine epochs of Atacama Large Millimeter/submillimeter Array (ALMA) observations of HOPS 358 taken over the course of the decline and subsequent rise in brightness seen with the JCMT to test whether the variation seen on ∼15″ scales, covering both disk and envelope, is also observed on smaller, <1″ scales that primarily probe HOPS 358’s protostellar disk. We detect both HOPS 358 and its southern companion, HOPS 358B, in our ALMA observations and find that at least one of the two is varying. Assuming that HOPS 358 is the variable, the light curve has the same shape as that found by the JCMT. Additionally, our high-resolution ALMA imaging of HOPS 358 reveals that the disk is warped, with a 16° warp at a disk radius of 35 au, about halfway through the extent of the disk. The physical origin of the warp and how it relates to the variability seen toward HOPS 358, however, remain unclear. |
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| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-6b43e4ee3dfe4f25b7789c37b6b9ee5e2025-08-20T02:10:46ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01982217610.3847/1538-4357/adaf9bSubmillimeter Variability in the Envelope and Warped Protostellar Disk of the Class 0 Protostar HOPS 358Patrick D. Sheehan0https://orcid.org/0000-0002-9209-8708Doug Johnstone1https://orcid.org/0000-0002-6773-459XCarlos Contreras Peña2https://orcid.org/0000-0003-1894-1880Seonjae Lee3https://orcid.org/0000-0001-6324-8482Gregory Herczeg4https://orcid.org/0000-0002-7154-6065Jeong-Eun Lee5https://orcid.org/0000-0003-3119-2087Steve Mairs6https://orcid.org/0000-0002-6956-0730John J. Tobin7https://orcid.org/0000-0002-6195-0152Hyeong-Sik Yun8https://orcid.org/0000-0001-6842-1555The JCMT Transient TeamNational Radio Astronomy Observatory , 520 Edgemont Rd., Charlottesville, VA 22903, USANRC Herzberg Astronomy and Astrophysics , 5071 West Saanich Rd., Victoria, BC V9E 2E7, Canada; Department of Physics and Astronomy, University of Victoria , Victoria, BC V8P 5C2, CanadaDepartment of Physics and Astronomy, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of Korea; Research Institute of Basic Sciences, Seoul National University , Seoul 08826, Republic of KoreaDepartment of Physics and Astronomy, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of KoreaKavli Institute for Astronomy and Astrophysics, Peking University , Yiheyuan Lu 5, Haidian Qu, 100871 Beijing, People’s Republic of China; Department of Astronomy, Peking University , Yiheyuan 5, Haidian Qu, 100871 Beijing, People’s Republic of ChinaDepartment of Physics and Astronomy, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of Korea; SNU Astronomy Research Center, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of KoreaNRC Herzberg Astronomy and Astrophysics , 5071 West Saanich Rd., Victoria, BC V9E 2E7, Canada; East Asian Observatory , 660 N. A‘ohōkū Place, Hilo, HI 96720, USANational Radio Astronomy Observatory , 520 Edgemont Rd., Charlottesville, VA 22903, USAKorea Astronomy and Space Science Institute , 776 Daedeok-daero, Yuseong, Daejeon 34055, Republic of KoreaThe James Clerk Maxwell Telescope (JCMT) Transient Survey recently discovered that the Class 0 protostar HOPS 358 decreased in 350 GHz continuum brightness by ∼25% over the course of 4 yr before brightening again for the next 4. The JCMT light curve can be fit by a long-timescale dip lasting roughly 8 yr. A shorter-timescale periodicity is also apparent with a period of 1.75 yr and a small 3% amplitude. NEOWISE monitoring reveals that the mid-infrared wavelength brightness of HOPS 358 follows a similar long-term pattern in time. Here, we present a study of nine epochs of Atacama Large Millimeter/submillimeter Array (ALMA) observations of HOPS 358 taken over the course of the decline and subsequent rise in brightness seen with the JCMT to test whether the variation seen on ∼15″ scales, covering both disk and envelope, is also observed on smaller, <1″ scales that primarily probe HOPS 358’s protostellar disk. We detect both HOPS 358 and its southern companion, HOPS 358B, in our ALMA observations and find that at least one of the two is varying. Assuming that HOPS 358 is the variable, the light curve has the same shape as that found by the JCMT. Additionally, our high-resolution ALMA imaging of HOPS 358 reveals that the disk is warped, with a 16° warp at a disk radius of 35 au, about halfway through the extent of the disk. The physical origin of the warp and how it relates to the variability seen toward HOPS 358, however, remain unclear.https://doi.org/10.3847/1538-4357/adaf9bProtostarsPre-main sequence starsStar formationProtoplanetary disks |
| spellingShingle | Patrick D. Sheehan Doug Johnstone Carlos Contreras Peña Seonjae Lee Gregory Herczeg Jeong-Eun Lee Steve Mairs John J. Tobin Hyeong-Sik Yun The JCMT Transient Team Submillimeter Variability in the Envelope and Warped Protostellar Disk of the Class 0 Protostar HOPS 358 The Astrophysical Journal Protostars Pre-main sequence stars Star formation Protoplanetary disks |
| title | Submillimeter Variability in the Envelope and Warped Protostellar Disk of the Class 0 Protostar HOPS 358 |
| title_full | Submillimeter Variability in the Envelope and Warped Protostellar Disk of the Class 0 Protostar HOPS 358 |
| title_fullStr | Submillimeter Variability in the Envelope and Warped Protostellar Disk of the Class 0 Protostar HOPS 358 |
| title_full_unstemmed | Submillimeter Variability in the Envelope and Warped Protostellar Disk of the Class 0 Protostar HOPS 358 |
| title_short | Submillimeter Variability in the Envelope and Warped Protostellar Disk of the Class 0 Protostar HOPS 358 |
| title_sort | submillimeter variability in the envelope and warped protostellar disk of the class 0 protostar hops 358 |
| topic | Protostars Pre-main sequence stars Star formation Protoplanetary disks |
| url | https://doi.org/10.3847/1538-4357/adaf9b |
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