J/AJ/165/72 IR water vapor emission from planet-forming disks (Banzatti+, 2023)
The Kinematics and Excitation of Infrared Water Vapor Emission from Planet-
forming Disks; Results from Spectrally Resolved Surveys and Guidelines for JWST
Spectra.
Banzatti A., Pontoppidan K.M., Chavez J.P., Salyk C., Diehl L.,
Bruderer S., Herczeg G.J., Carmona A., Pascucci I., Brittain S.,
Jensen S., Grant S., van Dishoeck E.F., Kamp I., Bosman A.D., Oberg K.I.,
Blake G.A., Meyer M.R., Gaidos E., Boogert A., Rayner J.T., Wheeler C.
<Astron. J., 165, 72 (2023)>
=2023AJ....165...72B 2023AJ....165...72B
ADC_Keywords: Exoplanets; Star Forming Region; Stars, pre-main sequence;
Spectra, infrared
Keywords: Circumstellar disks ; Protoplanetary disks ; Planet formation ;
Exoplanet formation ; Star formation ; Classical T Tauri stars
; Herbig Ae/Be stars ; Pre-main sequence stars ; High
resolution spectroscopy ; Molecular spectroscopy ; Infrared
astronomy ; Vibrational spectroscopy
Abstract:
This work presents ground-based spectrally resolved water emission at
R=30000-100000 over infrared wavelengths covered by the JWST
(2.9-12.8µm). Two new surveys with iSHELL and the VISIR are
combined with previous spectra from the CRIRES to cover parts of
multiple rovibrational and rotational bands observable within telluric
transmission bands, for a total of ∼160 spectra and 85 disks (30 of
which are JWST targets in Cycle 1). The general expectation of a range
of regions and excitation conditions traced by infrared water spectra
is for the first time supported by the combined kinematics and
excitation as spectrally resolved at multiple wavelengths. The main
findings from this analysis are: (1) water lines are progressively
narrower from the rovibrational bands at 2-9µm to the rotational
lines at 12µm, and partly match broad and narrow emission
components, respectively, as extracted from rovibrational CO spectra;
(2) rotation diagrams of resolved water lines from upper-level
energies of 4000-9500K show vertical spread and curvatures indicative
of optically thick emission (∼1018/cm2) from a range of excitation
temperatures (∼800-1100K); and (3) the new 5µm spectra demonstrate
that slab model fits to the rotational lines at >10µm strongly
overpredict the rovibrational emission bands at <9µm, implying
vibrational excitation not in thermodynamic equilibrium. We discuss
these findings in the context of emission from a disk surface and a
molecular inner disk wind, and provide a list of guidelines to support
the analysis of spectrally unresolved JWST spectra.
Description:
Water rovibrational emission spectra at 2.9-2.98µm are included as
observed with the Cryogenic High-Resolution IR Echelle Spectrograph
(CRIRES) on Very Large Telescope (VLT) as part of a survey from
2007-2008 (R=95000).
Water rovibrational emission spectra at 5µm are included as
observed with iSHELL at the NASA Infrared Telescope Facility (IRTF),
as part of an ongoing M-band survey of protoplanetary disks. iSHELL
covers a wide portion of the observable M band at 4.5∼5.25µm with a
resolution of 60000.
Water rotational emission spectra at 12.2-12.9µm were obtained
within a Large Program with VLT Imager and Spectrometer for the
Mid-Infrared (VISIR), (R=30000).
Additional water rotational emission spectra at 12.2-12.4µm are
included as obtained with Texas Echelon Cross Echelle Spectrograph
(TEXES) on Gemini with a resolving power of 100000.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 111 85 Sample and line flux measurements
table5.dat 102 34 Water line flux measurements from M-band iSHELL
spectra
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See also:
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
J/A+A/426/503 : Cat. of high velocity molecular outflows (Update) (Wu+ 2004)
J/A+A/432/369 : Leiden Atomic & Molecular Database (LAMDA) (Schoeier+, 2005)
J/A+A/492/257 : Collisional excitation of water in warm media (Faure+, 2008)
J/ApJ/703/1964 : Spectra of three nearby star-forming regions (Furlan+, 2009)
J/ApJ/769/21 : Accretion luminosities young stars Pfβ (Salyk+, 2013)
J/ApJ/786/97 : Photospheric properties of T Tauri stars (Herczeg+, 2014)
J/ApJ/845/44 : 340GHz SMA; 50 nearby protoplanetary disks (Tripathi+, 2017)
J/ApJ/869/L41 : DSHARP I. Sample, ALMA obs. log and overview (Andrews+, 2018)
J/ApJ/869/L42 : DSHARP. II. Annular substructures data (Huang+, 2018)
J/MNRAS/493/234 : Herbig Ae/Be accretion & mechanisms (Wichittanakom+ 2020)
J/A+A/650/A182 : Homogeneous study of Herbig Ae/Be stars (Guzman-Diaz+, 2021)
J/A+A/648/A19 : Spiral structure in the gas disc of CQ Tau (Woelfer+, 2021)
J/AJ/163/174 : IRTF/VLT M-band spectroscopic survey (Banzatti+, 2022)
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Object name
12- 14 I3 pc Dist [60/872]? Distance
16- 19 F4.1 --- S [1.3/15.1]? CO line shape parameter
21- 25 F5.1 Jy Fc(2.9) [0.2/896]? Continuum flux to calibrate
line flux at 2.9um
27- 34 E8.2 mW/m2/Jy Fcn(2.9) [7e-17/6e-14]? Continuum-normalized H2O
line flux at 2.9um
36- 43 E8.2 mW/m2/Jy e_Fcn(2.9) [1e-16/5e-14]? Uncertainty in Fcn(2.9)
45- 49 F5.1 Jy Fc(5) [0.2/951]? Continuum flux to calibrate
line flux at 5um
51- 59 E9.2 mW/m2/Jy Fcn(5) [-4e-15/2e-14]? Continuum-normalized H2O
line flux at 5um
61- 68 E8.2 mW/m2/Jy e_Fcn(5) [4e-17/3e-14]? Uncertainty in Fcn5
70- 78 E9.2 mW/m2/Jy Fcn(CO) [-5e-15/2e-13]? Continuum-normalized CO
line flux at 5um
80- 87 E8.2 mW/m2/Jy e_Fcn(CO) [1e-17/4e-14]? Uncertainty in Fcn(CO)
89- 92 F4.1 Jy Fc(12.4) [0.1/28]? Continuum flux to calibrate
line flux at 12.4um
94-102 E9.2 mW/m2/Jy Fcn(12.4) [-7e-15/2e-14]? Continuum-normalized H2O
line flux at 12.4um
104-111 E8.2 mW/m2/Jy e_Fcn(12.4) [5e-17/4e-14]? Uncertainty in Fcn(12.4)
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Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 --- ID Line identifier; v(upper-lower)JKaKc
(upper-lower)
24- 30 F7.5 um Wave [4.52/5.23] Line rest wavelength from
HITRAN database
32- 39 E8.2 mW/m2/Jy Fcn(AS205N) [1e-16/2e-14] Continuum-normalized line
flux in AS205N
41- 48 E8.2 mW/m2/Jy e_Fcn(AS205N) [3e-16/2e-14] Uncertainty in Fcn(AS205N)
50- 57 E8.2 mW/m2/Jy Fcn(DRTau) [1e-16/2e-14] Continuum-normalized line
flux in DRTau
59- 66 E8.2 mW/m2/Jy e_Fcn(DRTau) [2e-16/2e-14] Uncertainty in Fcn(DRTau)
68- 75 E8.2 mW/m2/Jy Fcn(FZTau) [2e-16/4e-14] Continuum-normalized line
flux in FZTau
77- 84 E8.2 mW/m2/Jy e_Fcn(FZTau) [4e-16/2e-14] Uncertainty in Fcn(FZTau)
86- 93 E8.2 mW/m2/Jy Fcn(CrA-IRS2) [2e-16/2e-14] Continuum-normalized line
flux in CrA-IRS2
95-102 E8.3 mW/m2/Jy e_Fcn(CrA-IRS2) [2e-16/2e-14] Uncertainty in
Fcn(CrA-IRS2)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 31-May-2023