First detection of CHD<sub>2</sub>OH towards pre-stellar cores

Lin, Yuxin; Spezzano, S.; Caselli, P.

doi:10.1051/0004-6361/202245524

Cited by 4 publications

(2 citation statements)

References 79 publications

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“…For HOPS 373SW, the column density ratio between CHD 2 OH and CH 2 DOH is 0.75, which is much higher than the ratio between CH 2 DOH and CH 3 OH. This trend is consistent with other hot corinos (Drozdovskaya et al 2022) and prestellar cores (Lin et al 2023). Figure 9 shows that Note.…”

Section: Deuteration Of Ch 3 Oh and Ch 3 Chosupporting

confidence: 89%

Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW

Lee,

Baek,

Lee

et al. 2023

ApJ

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We present the spectra of complex organic molecules (COMs) detected in HOPS 373SW with the Atacama Large Millimeter/submillimeter Array (ALMA). HOPS 373SW, which is a component of a protostellar binary with a separation of 1500au, has been discovered as a variable protostar by the JCMT transient monitoring survey with a modest (∼30%) brightness increase at submillimeter wavelengths. Our ALMA target-of-opportunity observation at ∼345 GHz for HOPS 373SW revealed extremely young chemical characteristics with strong deuteration of methanol. The dust continuum opacity is very high toward the source center, obscuring line emission from within 0.″03. The other binary component, HOPS 373NE, was detected only in C17O in our observation, implying a cold and quiescent environment. We compare the COM abundances relative to CH3OH in HOPS 373SW with those of V883 Ori, which is an eruptive disk object, as well as other hot corinos, to demonstrate the chemical evolution from envelope to disk. High abundances of singly, doubly, and triply deuterated methanol (CH2DOH, CHD2OH, and CD3OH) and a low CH3CN abundance in HOPS 373SW compared to other hot corinos suggest a very early evolutionary stage of HOPS 373SW in the hot corino phase. Since the COMs detected in HOPS 373SW would have been sublimated very recently from grain surfaces, HOPS 373SW is a promising place to study the surface chemistry of COMs in the cold prestellar phase before sublimation.

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Section: Deuteration Of Ch 3 Oh and Ch 3 Chosupporting

confidence: 89%

Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW

Lee,

Baek,

Lee

et al. 2023

ApJ

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“…On the other hand, our result in B335 is lower than the ratios in the other low-mass protostellar sources, NGC1333 IRAS 2A (0.70 ± 0.26), IRAS 4A (0.56 ± 0.22; Taquet et al 2019), and HOPS373SW (0.75;Lee et al 2023). Recently, the CHD 2 OH and CH 2 DOH lines were detected in the prestellar sources as well, the ratios being 0.8 ± 0.4 in H-MM1 and 0.5 ± 0.3 in L694-2 (Lin et al 2023). Furthermore, the D/H ratio from CHD 2 OH and CH 2 DOH is reported to be higher than that from CH 2 DOH and CH 3 OH in the above protostellar and prestellar sources (Appendix E).…”

Section: [Chd 2 Oh]/[ch 2 Doh]mentioning

confidence: 97%

CH₃OH and Its Deuterated Species in the Disk/Envelope System of the Low-mass Protostellar Source B335

Okoda,

Oya,

Sakai

et al. 2024

ApJ

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Deuterium fractionation in the closest vicinity of a protostar is important in understanding its potential heritage to a planetary system. Here, we have detected the spectral line emission of CH3OH and its three deuterated species, CH2DOH, CHD2OH, and CH3OD, toward the low-mass protostellar source B335 at a resolution of 0.″03 (5 au) with Atacama Large Millimeter/submillimeter Array. They have a ring distribution within the radius of 24 au with the intensity depression at the continuum peak. We derive the column densities and abundance ratios of the above species at six positions in the disk/envelope system as well as the continuum peak. The D/H ratio of CH3OH is ∼[0.03–0.13], which is derived by correcting the statistical weight of 3 for CH2DOH. The [CHD2OH]/[CH2DOH] ratio is derived to be higher ([0.14–0.29]). On the other hand, the [CH2DOH]/[CH3OD] ratio ([4.9–15]) is higher than the statistical ratio of 3 and is comparable to those reported for other low-mass sources. We study the physical structure on a few astronomical unit scales in B335 by analyzing the CH3OH (183,15 − 182,16, A) and HCOOH (120,12 − 110,11) line emission. Velocity structures of these lines are reasonably explained as the infalling-rotating motion. The protostellar mass and the upper limit to the centrifugal barrier are thus derived to be 0.03–0.07 M ⊙ and <7 au, respectively, showing that B335 harbors a young protostar with a tiny disk structure. Such youth of the protostar may be related to the relatively high [CH2DOH]/[CH3OH] ratio.

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Investigation of the rotational spectrum of CD₃OD and an astronomical search toward IRAS 16293-2422

Ilyushin¹,

Müller²,

Jørgensen³

et al. 2023

A&A

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Solar-type prestellar cores and protostars frequently display large amounts of deuterated organic molecules and, in particular, high relative abundances of doubly and triply deuterated isotopologs. Recent findings on CHD2OH and CD3OH toward IRAS 16293–2422 suggest that even fully deuterated methanol, CD3OD, may be detectable as well. However, searches for CD3OD are hampered in particular by the lack of intensity information from a spectroscopic model. The objective of the present investigation is to develop a spectroscopic model of CD3OD in low-lying torsional states that is sufficiently accurate to facilitate searches for this isotopolog in space. We carried out a new measurement campaign for CD3OD involving two spectroscopic laboratories that covers the 34 GHz–1.1 THz range. A torsion-rotation Hamiltonian model based on the rho-axis method was employed for our analysis. Our resulting model describes the ground and first excited torsional states of CD3OD well up to quantum numbers J ⩽ 51 and Ka ⩽ 23. We derived a line list for radio-astronomical observations from this model that is accurate up to at least 1.1 THz and should be sufficient for all types of radio-astronomical searches for this methanol isotopolog. This line list was used to search for CD3OD in data from the Protostellar Interferometric Line Survey of IRAS 16293–2422 obtained with the Atacama Large Millimeter/submillimeter Array. While we found several emission features that can be attributed largely to CD3OD, their number is still not sufficiently high enough to establish a clear detection. Nevertheless, the estimate of 2 × 1015 cm−2 derived for the CD3OD column density may be viewed as an upper limit that can be compared to column densities of CD3OH, CH3OD, and CH3OH. The comparison indicates that the CD3OD column density toward IRAS 16293–2422 is in line with the enhanced D/H ratios observed for multiply deuterated complex organic molecules.

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First detection of CHD₂OH towards pre-stellar cores

Cited by 4 publications

References 79 publications

Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW

Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW

CH₃OH and Its Deuterated Species in the Disk/Envelope System of the Low-mass Protostellar Source B335

Investigation of the rotational spectrum of CD₃OD and an astronomical search toward IRAS 16293-2422

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First detection of CHD2OH towards pre-stellar cores

Cited by 4 publications

References 79 publications

Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW

Complex Organic Molecules in a Very Young Hot Corino, HOPS 373SW

CH3OH and Its Deuterated Species in the Disk/Envelope System of the Low-mass Protostellar Source B335

Investigation of the rotational spectrum of CD3OD and an astronomical search toward IRAS 16293-2422

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First detection of CHD₂OH towards pre-stellar cores

CH₃OH and Its Deuterated Species in the Disk/Envelope System of the Low-mass Protostellar Source B335

Investigation of the rotational spectrum of CD₃OD and an astronomical search toward IRAS 16293-2422