ALMA high-resolution observations unveil planet formation shaping molecular emission in the PDS 70 disk

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Volume 689 (September 2024)

A&A, 689 (2024) A65

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Table 1

Listed imaged lines, corresponding rest frequencies, imaging parameters (channel width, beam, RMS), and line fluxes.

Species	Transition^(a)	Frequency [GHz]	Δυ [km s⁻¹]	Beam	RMS [mJy beam⁻¹]	Flux^(b) [mJy km s⁻¹]	Velocity range^(c) [km s⁻¹]	ϵ factor
¹²CO	2–1	230.5380	0.1	$0_{\cdot}^{''} 28 × 0_{\cdot}^{''} 22$ $\[0^{\prime\prime}_\cdot 28\text { \times }0^{\prime\prime}_\cdot 22\]$	0.54	6175 ± 23	0.0–10.3	0.30
¹³CO	2–1	220.3986	0.2	$0_{\cdot}^{''} 30 × 0_{\cdot}^{''} 24$ $\[0^{\prime\prime}_\cdot 30\text { \times }0^{\prime\prime}_\cdot 24\]$	0.42	1859 ± 12	1.7–9.1	0.32
C¹⁸O	2–1	219.5603	0.2	$0_{\cdot}^{''} 31 × 0_{\cdot}^{''} 24$ $\[0^{\prime\prime}_\cdot 31\text { \times }0^{\prime\prime}_\cdot 24\]$	0.33	466 ± 7	2.1–8.5	0.31
H₂CO	3₀_,3−2₀_,2	218.2221	0.4	$0_{\cdot}^{''} 29 × 0_{\cdot}^{''} 23$ $\[0^{\prime\prime}_\cdot 29\text { \times }0^{\prime\prime}_\cdot 23\]$	0.19	708 ± 7	1.9–9.1	0.30
H₂CO	3_2,1−2_2,0	218.7600	0.4	$0_{\cdot}^{''} 29 × 0_{\cdot}^{''} 23$ $\[0^{\prime\prime}_\cdot 29\text { \times }0^{\prime\prime}_\cdot 23\]$	0.20	57 ± 6	2.7–8.3	0.30
C₂H	3_7/2,4−2_5/2,3	262.0042	0.4	$0_{\cdot}^{''} 20 × 0_{\cdot}^{''} 15$ $\[0^{\prime\prime}_\cdot 20\text { \times }0^{\prime\prime}_\cdot 15\]$	0.16	723 ± 10	0–9.1^(d)	0.23
C₂H	3_7/2,3−2_5/2,2	262.0064	0.4	$0_{\cdot}^{''} 20 × 0_{\cdot}^{''} 15$ $\[0^{\prime\prime}_\cdot 20\text { \times }0^{\prime\prime}_\cdot 15\]$	0.16	577 ± 10	0–9.1^(d)	0.23
H¹³CN	3–2	259.0117	0.4	$0_{\cdot}^{''} 20 × 0_{\cdot}^{''} 15$ $\[0^{\prime\prime}_\cdot 20\text { \times }0^{\prime\prime}_\cdot 15\]$	0.13	360 ± 8	1.9–9.1	0.22
HC¹⁵N	3–2	258.1571	0.4	$0_{\cdot}^{''} 20 × 0_{\cdot}^{''} 15$ $\[0^{\prime\prime}_\cdot 20\text { \times }0^{\prime\prime}_\cdot 15\]$	0.15	176 ± 7	2.7–8.3	0.22
DCN	3–2	217.2386	0.4	$0_{\cdot}^{''} 29 × 0_{\cdot}^{''} 23$ $\[0^{\prime\prime}_\cdot 29\text { \times }0^{\prime\prime}_\cdot 23\]$	0.22	230 ± 6	2.3–8.7	0.30
H¹³CO⁺	3–2	260.2553	0.4	$0_{\cdot}^{''} 21 × 0_{\cdot}^{''} 15$ $\[0^{\prime\prime}_\cdot 21\text { \times }0^{\prime\prime}_\cdot 15\]$	0.16	372 ± 7	2.3–8.7	0.23
CS	5–4	244.9355	1.4	$0_{\cdot}^{''} 22 × 0_{\cdot}^{''} 15$ $\[0^{\prime\prime}_\cdot 22\text { \times }0^{\prime\prime}_\cdot 15\]$	0.06	445 ± 6	2.7–8.3	0.23
c-C₃H₂	3_2,1−2_1,2	244.2221	1.4	$0_{\cdot}^{''} 22 × 0_{\cdot}^{''} 16$ $\[0^{\prime\prime}_\cdot 22\text { \times }0^{\prime\prime}_\cdot 16\]$	0.07	16 ± 2	1.3–9.7	0.52
c-C₃H₂	7_1,6−7₀_,7	218.7327	0.4	$0_{\cdot}^{''} 29 × 0_{\cdot}^{''} 23$ $\[0^{\prime\prime}_\cdot 29\text { \times }0^{\prime\prime}_\cdot 23\]$	0.20	10 ± 3^(e)	1.5–8.3	0.52
c-C₃H₂	7_2,6−7_1,7	218.7327	0.4	$0_{\cdot}^{''} 29 × 0_{\cdot}^{''} 23$ $\[0^{\prime\prime}_\cdot 29\text { \times }0^{\prime\prime}_\cdot 23\]$	0.69	10 ± 3^(e)	1.5–8.3	0.52
SO	6₇−5₆	261.8436	0.2	$0_{\cdot}^{''} 20 × 0_{\cdot}^{''} 15$ $\[0^{\prime\prime}_\cdot 20\text { \times }0^{\prime\prime}_\cdot 15\]$	0.91	<149^(f⁾	1.9–9.1^(g)	−
SO	6₆−5₅	258.2558	0.5	$0_{\cdot}^{''} 21 × 0_{\cdot}^{''} 15$ $\[0^{\prime\prime}_\cdot 21\text { \times }0^{\prime\prime}_\cdot 15\]$	0.66	<106^(f⁾	2.0–9.0^(g)	−
CH₃OH	5_1,4,0−4_1,3,0	243.9157	1.5	$0_{\cdot}^{''} 22 × 0_{\cdot}^{''} 16$ $\[0^{\prime\prime}_\cdot 22\text { \times }0^{\prime\prime}_\cdot 16\]$	0.29	<118^(f⁾	1.0–10.0^(g)	−

Notes. ^(a)Quantum numbers are formatted for H₂CO (CDMS, Chardon & Guichon 1973; Müller & Lewen 2017), c-C₃H₂ (CDMS, Bogey et al. 1986; Vrtilek et al. 1987; Lovas et al. 1992) as $N_{K_{a}, K_{c}}$ $\[N_{K_a, K_c}\]$ , for C₂H as $N_{J, F_{1}}$ $\[N_{J, F_1}\]$ (CDMS, Sastry et al. 1981; Müller et al. 2000; Padovani et al. 2009), for SO as N_J (Amano & Hirota 1974; Clark & De Lucia 1976; Tiemann 1982; Lovas et al. 1992, CDMS), for CH₃OH as $N_{K_{a}, K_{c}, v}$ $\[N_{K_a, K_c, v}\]$ (CDMS, Xu et al. 2008; Lees & Baker 1968; Pickett et al. 1981; Sastry et al. 1984; Herbst et al. 1984), for ¹²CO (CDMS, Winnewisser et al. 1997), ¹³CO (CDMS, Klapper et al. 2000; Cazzoli et al. 2004), C¹⁸O (CDMS, Winnewisser et al. 1985), H¹³CN (CDMS, Fuchs et al. 2004; Cazzoli & Puzzarini 2005; Maiwald et al. 2000), HC¹⁵N (CDMS, Fuchs et al. 2004; Cazzoli & Puzzarini 2005), DCN (CDMS, Brünken et al. 2004), H¹³CO⁺ (CDMS, Gregersen & Evans 2001; Lattanzi et al. 2007), CS (CDMS, Müller et al. 2005; Bogey et al. 1981; Ahrens & Winnewisser 1999) as J. ^(b)The uncertainty does not include the 10% absolute flux calibration. ^(c) Velocity range over which the spectral integration has been performed to evaluate the flux (chosen after visual inspection of the data, to include channel maps where signal is detected). ^(d)Limits of the integration performed after the double-Gaussian fit to the hyperfine components of the spectrum. ^(e)The value refers to the total flux of the blended c-C₃H₂ (218 GHz) lines. ^(f)Upper limit on the integrated flux evaluated from the integrated intensity maps, as 3 times the standard deviation of the flux of 26 de-projected circles, taken outside the possible emitting region, with a radius of 2″.^(g) Velocity range over which we extracted the integrated intensity maps, from which the indicated upper limit on the line flux has been estimated. The range has been selected to match the average one from detected lines, compatible with the channel width of cubes of undetected lines.

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