Implications of a Hot Atmosphere/Corino from ALMA Observations toward NGC 1333 IRAS 4A1

Sahu, Dipen; Liu, Sheng-Yuan; Su, Yu‐Nung; Li, Zhi-Yun; Lee, Chin-Fei; Hirano, Naomi; Takakuwa, Shigehisa

doi:10.3847/1538-4357/aaffda

Cited by 41 publications

(56 citation statements)

References 89 publications

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“…The first hot corino was discovered in 2003 toward the Class 0 source IRAS 16293-2422 (e.g., Cazaux et al 2003;Jørgensen et al 2016;Manigand et al 2020). Since then other Class 0 hot corinos have been discovered: NGC 1333 IRAS 4A (hereafter IRAS 4A; e.g., Bottinelli et al 2004;Taquet et al 2015;De Simone et al 2017;López-Sepulcre et al 2017;Sahu et al 2019), NGC 1333 IRAS 2A, NGC 1333 IRAS 4B (e.g., Jørgensen et al 2005;Bottinelli et al 2007;Maury et al 2014;De Simone et al 2017), HH 212 (Codella et al 2016;Bianchi et al 2017;Lee et al 2017Lee et al , 2019, B335 (Imai et al 2016), L483 (Oya et al 2017;Jacobsen et al 2019), Barnard1b-S (Marcelino et al 2018), Ser-emb 1 (Martin-Domenech et al 2019), and BHR71-IRS1 (Yang et al 2020). Lately, a few more evolved Class I hot corinos were also discovered: NGC 1333 SVS13A (De Simone et al 2017;Bianchi et al 2019), B1a (Öberg et al 2014), and Ser-emb 17 (Bergner et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Hot Corinos Chemical Diversity: Myth or Reality?

Simone

Ceccarelli

Codella

et al. 2020

ApJL

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After almost 20 years of hunting, only about a dozen hot corinos, hot regions enriched in interstellar complex organic molecules (iCOMs), are known. Of them, many are binary systems with the two components showing drastically different molecular spectra. Two obvious questions arise. Why are hot corinos so difficult to find and why do their binary components seem chemically different? The answer to both questions could be a high dust opacity that would hide the molecular lines. To test this hypothesis, we observed methanol lines at centimeter wavelengths, where dust opacity is negligible, using the Very Large Array interferometer. We targeted the NGC 1333 IRAS 4A binary system, for which one of the two components, 4A1, has a spectrum deprived of iCOMs lines when observed at millimeter wavelengths, while the other component, 4A2, is very rich in iCOMs. We found that centimeter methanol lines are similarly bright toward 4A1 and 4A2. Their non-LTE analysis indicates gas density and temperature (2 10 6 cm −3 and 100-190 K), methanol column density (∼10 19 cm −2), and extent (∼35 au in radius) similar in 4A1 and 4A2, proving that both are hot corinos. Furthermore, the comparison with previous methanol line millimeter observations allows us to estimate the optical depth of the dust in front of 4A1 and 4A2, respectively. The obtained values explain the absence of iCOMs line emission toward 4A1 at millimeter wavelengths and indicate that the abundances toward 4A2 are underestimated by ∼30%. Therefore, centimeter observations are crucial for the correct study of hot corinos, their census, and their molecular abundances.

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Section: Introductionmentioning

confidence: 99%

Hot Corinos Chemical Diversity: Myth or Reality?

Simone

Ceccarelli

Codella

et al. 2020

ApJL

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“…For IRAS4A2, the observed polarization percentage is below the predicted model as shown in Figure 2(f). This may partly due to that there are a forest of spectral lines (Sahu et al 2019), which leads to an overestimate of stoke I continuum flux and consequently an underestimate of polarization percentage. For comparison, we have also done the similar evaluation but assuming a constant T dust = 20 K, which is shown as the blue curve in Figure 2(b).…”

Section: Discussionmentioning

confidence: 99%

Resolving Linear Polarization due to Emission and Extinction of Aligned Dust Grains on NGC 1333 IRAS4A with JVLA and ALMA

Liu

Lai

et al. 2020

ApJ

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We report high angular resolution observations of linearly polarized dust emission towards the Class 0 young stellar object (YSO) NGC1333 IRAS4A (hereafter, IRAS4A) using the Karl G. Jansky Very Large Array (JVLA) at K (11.5-16.7 mm), Ka (8.1-10.3 mm), and Q bands (6.3-7.9 mm), and using the Atacama Large Millimeter Array (ALMA) at Band 6 (1.2 mm) and Band 7 (0.85-0.89 mm). On 100-1000 AU scales, all of these observations consistently trace the hourglass shaped magnetic field topology as shown in the previous studies. In the innermost 100 AU region of IRAS4A1, the polarization position angles (E-field) detected at 6.3-16.7 mm are consistent, however, are nearly 90 degrees offset from those detected at 1.2 mm and 0.85-0.89 mm. Such a 90 degree offset may be explained by that the inner ∼100 AU area is optically thick at wavelengths shorter than ∼1.5 mm, whereby the observations probe the absorption of aligned dust against the weakly or unpolarized warm dust emission from the innermost region. This can also consistently explain why the highest angular resolution ALMA images at Band 7 show that the polarization percentage increases with dust brightness temperature in the inner ∼100 AU region of IRAS4A1. Following this interpretation and assuming that the dust grains are aligned with the magnetic fields, the inferred magnetic field position angle based on the 90 • rotated at 6.3-7.9 mm in the central peak of IRAS4A1 is ∼ −22 • , which is approximately consistent with the outflow direction ∼ −9 • .

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“…As the gas-to-dust ratios may vary across star-forming regions, and also between individual components of such systems, it is not always obvious when dust opacity starts to play a role in a frequency-dependent fashion (τ ν ∝ ν β , where ν is the frequency and β is the dust opacity exponent). Severe examples of dust optical thickness at submm ALMA Band 7 frequencies to the point that the majority of observed lines appear in absorption were seen on-source B in IRAS 16293-2422 (Jørgensen et al 2016) and on-source in NGC 1333-IRAS 4A1 (Sahu et al 2019). Dust extinction has also been reported to play a role in Orion KL Herschel/HIFI observations (Neill et al 2013).…”

Section: B3 Optical Thicknessmentioning

confidence: 96%

“…For NGC 1333-IRAS 4A, interferometric IRAM Plateau de Bure Interferometer (IRAM-PdBI; now called the NOrthern Extended Millimeter Array, NOEMA) observations determined a CH 2 DOH/CH 3 OH ratio of 0.037 (Taquet et al 2019). Subsequent interferometric ALMA observations separated the source into its binary components A1 and A2 with ratios of 0.0058 and 0.048, respectively (Sahu et al 2019), indicating that the two binary components are starkly different from one another (and that earlier IRAM-PdBI observations were dominated by the emission from A2). In protostellar regions, methanol is likely present in the extended cold circumstellar/circumbinary envelope, as well as on the most inner hot regions in the vicinity of the protostar(s).…”

Section: B1 Spatial Distributionmentioning

confidence: 99%

“…CH 3 OH gas is thought to always be optically thick (e.g. Menten et al 1988;Parise et al 2006;Neill et al 2013;Fuente et al 2014;Jørgensen et al 2016;Bianchi et al 2017a,b;Jørgensen et al 2018;Bøgelund et al 2018;Ospina-Zamudio et al 2018;Taquet et al 2019;Lee et al 2019;Sahu et al 2019;Agúndez et al 2019;Manigand et al 2020). For some sources, even the singly deuterated isotopologues (as for onsource in NGC 1333-IRAS 2A and -IRAS 4A for CH 2 DOH and CH 3 OD, Taquet et al 2019; or as for CH 2 DOH already at a half-0.5 arcsec-beam offset position from source B in IRAS 16293-2422, Jørgensen et al 2018) and the 13 C-isotopologue may be (partially) optically thick (as in NGC 6334I, Bøgelund et al 2018; or in Sagittarius B2(N2), Müller et al 2016; or at a half-0.5 arcsec-beam offset position from source B in IRAS 16293-2422, Jørgensen et al 2016Jørgensen et al , 2018.…”

Section: B3 Optical Thicknessmentioning

confidence: 99%

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Prestellar grain-surface origins of deuterated methanol in comet 67P/Churyumov–Gerasimenko

Drozdovskaya

Schroeder

Rubin

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Deuterated methanol is one of the most robust windows astrochemists have on the individual chemical reactions forming deuterium-bearing molecules and the physicochemical history of the regions where they reside. The first-time detection of mono- and di-deuterated methanol in a cometary coma is presented for comet 67P/Churyumov–Gerasimenko using Rosetta–ROSINA data. D-methanol (CH3OD and CH2DOH combined) and D2-methanol (CH2DOD and CHD2OH combined) have an abundance of 5.5 ± 0.46 and 0.00069 ± 0.00014 per cent relative to normal methanol. The data span a methanol deuteration fraction (D/H ratio) in the 0.71 − 6.6 per cent range, accounting for statistical corrections for the location of D in the molecule and including statistical error propagation in the ROSINA measurements. It is argued that cometary CH2DOH forms from CO hydrogenation to CH3OH and subsequent H-D substitution reactions in CH3-R. CHD2OH is likely produced from deuterated formaldehyde. Meanwhile, CH3OD and CH2DOD, could form via H-D exchange reactions in OH-R in the presence of deuterated water ice. Methanol formation and deuteration is argued to occur at the same epoch as D2O formation from HDO, with formation of mono-deuterated water, hydrogen sulfide, and ammonia occurring prior to that. The cometary D-methanol/methanol ratio is demonstrated to agree most closely with that in prestellar cores and low-mass protostellar regions. The results suggest that cometary methanol stems from the innate cold (10 − 20 K) prestellar core that birthed our Solar System. Cometary volatiles individually reflect the evolutionary phases of star formation from cloud to core to protostar.

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Implications of a Hot Atmosphere/Corino from ALMA Observations toward NGC 1333 IRAS 4A1

Cited by 41 publications

References 89 publications

Hot Corinos Chemical Diversity: Myth or Reality?

Hot Corinos Chemical Diversity: Myth or Reality?

Resolving Linear Polarization due to Emission and Extinction of Aligned Dust Grains on NGC 1333 IRAS4A with JVLA and ALMA

Prestellar grain-surface origins of deuterated methanol in comet 67P/Churyumov–Gerasimenko

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