The article ‘Confirmation of interstellar phosphine towards asymptotic giant branch star IRC<InlineEquation ID="IEq5"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq2.gif" Format="GIF" Height="13" Rendition="HTML" Resolution="72" Type="Linedraw" Width="14" /> </InlineMediaObject> <EquationSource Format="TEX">$+$</EquationSource> <EquationSource Format="MATHML"><math> <mo>+</mo> </math></EquationSource> </InlineEquation>10216’ by A. Manna and S. Pal uses ALMA data of the C-star envelope IRC<InlineEquation ID="IEq6"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq2.gif" Format="GIF" Height="13" Rendition="HTML" Resolution="72" Type="Linedraw" Width="14" /> </InlineMediaObject> <EquationSource Format="TEX">$+$</EquationSource> <EquationSource Format="MATHML"><math> <mo>+</mo> </math></EquationSource> </InlineEquation>10216 to claim a confirmation of the detection of <InlineEquation ID="IEq7"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq1.gif" Format="GIF" Height="16" Rendition="HTML" Resolution="72" Type="Linedraw" Width="31" /> </InlineMediaObject> <EquationSource Format="TEX">$\hbox {PH}_3$</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mtext>PH</mtext> <mn>3</mn> </msub> </math></EquationSource> </InlineEquation> in this source. The article, however, incorrectly assigns an emission feature observed in the ALMA spectrum of IRC<InlineEquation ID="IEq8"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq2.gif" Format="GIF" Height="13" Rendition="HTML" Resolution="72" Type="Linedraw" Width="14" /> </InlineMediaObject> <EquationSource Format="TEX">$+$</EquationSource> <EquationSource Format="MATHML"><math> <mo>+</mo> </math></EquationSource> </InlineEquation>10216 to <InlineEquation ID="IEq9"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq1.gif" Format="GIF" Height="16" Rendition="HTML" Resolution="72" Type="Linedraw" Width="31" /> </InlineMediaObject> <EquationSource Format="TEX">$\hbox {PH}_3$</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mtext>PH</mtext> <mn>3</mn> </msub> </math></EquationSource> </InlineEquation>, while we find that it arises from a highly vibrationally excited state of HCN. Concretely the feature can be confidently assigned to the <InlineEquation ID="IEq10"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq10.gif" Format="GIF" Height="14" Rendition="HTML" Resolution="72" Type="Linedraw" Width="42" /> </InlineMediaObject> <EquationSource Format="TEX">$J=3$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>J</mi> <mo>=</mo> <mn>3</mn> </mrow> </math></EquationSource> </InlineEquation>–2, <InlineEquation ID="IEq11"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq11.gif" Format="GIF" Height="14" Rendition="HTML" Resolution="72" Type="Linedraw" Width="39" /> </InlineMediaObject> <EquationSource Format="TEX">$\ell =0$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>ℓ</mi> <mo>=</mo> <mn>0</mn> </mrow> </math></EquationSource> </InlineEquation> transition of HCN in the <InlineEquation ID="IEq12"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq12.gif" Format="GIF" Height="16" Rendition="HTML" Resolution="72" Type="Linedraw" Width="59" /> </InlineMediaObject> <EquationSource Format="TEX">$\nu _1 + 4\nu _2$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <msub> <mi>ν</mi> <mn>1</mn> </msub> <mo>+</mo> <mn>4</mn> <msub> <mi>ν</mi> <mn>2</mn> </msub> </mrow> </math></EquationSource> </InlineEquation> vibrational state based on the observation of the <InlineEquation ID="IEq13"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq13.gif" Format="GIF" Height="15" Rendition="HTML" Resolution="72" Type="Linedraw" Width="51" /> </InlineMediaObject> <EquationSource Format="TEX">$\ell = +2$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>ℓ</mi> <mo>=</mo> <mo>+</mo> <mn>2</mn> </mrow> </math></EquationSource> </InlineEquation> and <InlineEquation ID="IEq14"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq14.gif" Format="GIF" Height="15" Rendition="HTML" Resolution="72" Type="Linedraw" Width="52" /> </InlineMediaObject> <EquationSource Format="TEX">$\ell = -2$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>ℓ</mi> <mo>=</mo> <mo>-</mo> <mn>2</mn> </mrow> </math></EquationSource> </InlineEquation> components of the same rotational transition, <InlineEquation ID="IEq15"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq10.gif" Format="GIF" Height="14" Rendition="HTML" Resolution="72" Type="Linedraw" Width="42" /> </InlineMediaObject> <EquationSource Format="TEX">$J=3$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>J</mi> <mo>=</mo> <mn>3</mn> </mrow> </math></EquationSource> </InlineEquation>–2, with the observed relative intensities in agreement with the relative line strengths. The detection of <InlineEquation ID="IEq16"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq1.gif" Format="GIF" Height="16" Rendition="HTML" Resolution="72" Type="Linedraw" Width="31" /> </InlineMediaObject> <EquationSource Format="TEX">$\hbox {PH}_3$</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mtext>PH</mtext> <mn>3</mn> </msub> </math></EquationSource> </InlineEquation> in IRC<InlineEquation ID="IEq17"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq2.gif" Format="GIF" Height="13" Rendition="HTML" Resolution="72" Type="Linedraw" Width="14" /> </InlineMediaObject> <EquationSource Format="TEX">$+$</EquationSource> <EquationSource Format="MATHML"><math> <mo>+</mo> </math></EquationSource> </InlineEquation>10216 remains confirmed based on the observation of the <InlineEquation ID="IEq18"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq18.gif" Format="GIF" Height="14" Rendition="HTML" Resolution="72" Type="Linedraw" Width="42" /> </InlineMediaObject> <EquationSource Format="TEX">$J=1$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>J</mi> <mo>=</mo> <mn>1</mn> </mrow> </math></EquationSource> </InlineEquation>–0 and <InlineEquation ID="IEq19"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10058_Article_IEq19.gif" Format="GIF" Height="14" Rendition="HTML" Resolution="72" Type="Linedraw" Width="42" /> </InlineMediaObject> <EquationSource Format="TEX">$J=2$</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>J</mi> <mo>=</mo> <mn>2</mn> </mrow> </math></EquationSource> </InlineEquation>–1 lines with the single-dish telescopes IRAM 30m, ARO SMT 10m, and Herschel (Agúndez et al. 2008, 2014; Tenenbaum & Ziurys 2008).

Re-evaluation of ALMA detection of circumstellar $\hbox {PH}_3$ in the AGB envelope IRC$+$10216: Evidence for misidentification with HCN

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发表日期：

2025年5月31日

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M. Agúndez,
L. Velilla-Prieto,
J. P. Fonfría,
J. Cernicharo

摘要

The article ‘Confirmation of interstellar phosphine towards asymptotic giant branch star IRC $+$ $+$ 10216’ by A. Manna and S. Pal uses ALMA data of the C-star envelope IRC $+$ $+$ 10216 to claim a confirmation of the detection of $\hbox {PH}_3$ ${PH}_{3}$ in this source. The article, however, incorrectly assigns an emission feature observed in the ALMA spectrum of IRC $+$ $+$ 10216 to $\hbox {PH}_3$ ${PH}_{3}$ , while we find that it arises from a highly vibrationally excited state of HCN. Concretely the feature can be confidently assigned to the $J=3$ $J = 3$ –2, $\ell =0$ $ℓ = 0$ transition of HCN in the $\nu _1 + 4\nu _2$ $ν_{1} + 4 ν_{2}$ vibrational state based on the observation of the $\ell = +2$ $ℓ = + 2$ and $\ell = -2$ $ℓ = - 2$ components of the same rotational transition, $J=3$ $J = 3$ –2, with the observed relative intensities in agreement with the relative line strengths. The detection of $\hbox {PH}_3$ ${PH}_{3}$ in IRC $+$ $+$ 10216 remains confirmed based on the observation of the $J=1$ $J = 1$ –0 and $J=2$ $J = 2$ –1 lines with the single-dish telescopes IRAM 30m, ARO SMT 10m, and Herschel (Agúndez et al. 2008, 2014; Tenenbaum & Ziurys 2008).

Re-evaluation of ALMA detection of circumstellar \(\hbox {PH}_3\) in the AGB envelope IRC\(+\)10216: Evidence for misidentification with HCN

摘要