Table 2 contains measured rotational transitions and residuals from the fit for the two isomers of C-cyanomethanimine in the ground state. (1 data file)

Bachiller, R.

Barone, V.

Ceccarelli, C.

Cernicharo, J.

CODELLA, CLAUDIO

Degli Esposti, C.

Dore, L.

Lefloch, B.

Melli, A.

Melosso, M.

Puzzarini, C.

Spada, L.

OA@INAF - Istituto Nazionale di Astrofisica

2017Publication Year2020-09-15T15:21:42ZAcceptance in OA@INAFVizieR Online Data Catalog: Lab measurements for C-cyanomethanimine (Melosso+, 2018)TitleMelosso, M.; Melli, A.; Puzzarini, C.; CODELLA, CLAUDIO; Spada, L.; et al.Authors10.26093/cds/vizier.36090121DOIhttp://hdl.handle.net/20.500.12386/27387HandleVizieR Online Data CatalogJournalJ/A+A/609/A121        Lab measurements for C-cyanomethanimine   (Melosso+, 2018)Laboratory measurements and astronomical search for cyanomethanimine.    Melosso M., Melli A., Puzzarini C., Codella C., Spada L., Dore L.,    Degli Esposti C., Lefloch B., Bachiller R., Ceccarelli C., Cernicharo J.,    Barone V.    <Astron. Astrophys. 609, A121 (2018)>    =2018A&A...609A.121M        (SIMBAD/NED BibCode)ADC_Keywords: Atomic physics ; Interstellar mediumKeywords: ISM: molecules - molecular data - methods: data analysis -          methods: laboratory: molecularAbstract:    C-cyanomethanimine (HNCHCN), existing in the two Z and E isomeric    forms, is a key prebiotic molecule, but, so far, only the E isomer has    been detected towards the massive star forming region Sagittarius    B2(N) using transitions in the radio wavelength domain.    With the aim of detecting HNCHCN in Sun-like star-forming regions, the    laboratory investigation of its rotational spectrum has been extended    to the milllimeter-/submillimeter-wave (mm-/submm-) spectral window    where several unbiased spectral surveys have been already obtained.    High-resolution laboratory measurements of the rotational spectrum of    C-cyanomethanimine were carried out in the 100-420GHz range using a    frequency-modulation absorption spectrometer. The C-cyanomethanimine    spectral features were then searched for in the mm-wave range using    the high-sensitivity and unbiased spectral surveys obtained with the    IRAM 30-m antenna in the ASAI context, the earliest stages of star    formation from starless to evolved Class I objects being sampled.    For both the Z and E isomers, the spectroscopic work has led to an    improved and extended knowledge of the spectroscopic parameters, thus    providing accurate predictions of the rotational signatures up to    ∼700GHz. So far, no C-cyanomethanimine emission has been detected    towards the ASAI targets, and upper limits on the column density of    1011-1012cm-2 could only be derived. Consequently, the    C-cyanomethanimine abundances have to be less than a few 10-10 for    starless and hot-corinos. A less stringent constraint, ≤10-9, is    obtained for shocks sites. The combination of the upper limits on the    abundances of C-cyanomethanimine together with accurate laboratory    frequencies up to ∼700GHz poses the basis for future higher    sensitivity searches around Sun-like star forming regions. For compactJ/A+A/609/A121 https://cdsarc.unistra.fr/viz-bin/ReadMe/J/A+A/609/A121?format=html&tex=true1 di 3 15/09/2020, 17:21    (typically less than 1 arcsec) and chemically enriched sources such as    hot-corinos, the use of interferometers as NOEMA and ALMA in their    extended configurations are clearly needed.Description:    Table 2 contains measured rotational transitions and residuals from    the fit for the two isomers of C-cyanomethanimine in the ground state.File Summary:       FileName      Lrecl  Records   ExplanationsReadMe            80        .   This filetable2.dat        80     1185   Measured rotational transitions and residuals                                 from the fit for the two isomers of                                 C-cyanomethanimine in the ground stateSee also:J/A+A/562/A56 : Cyanomethyl anion & its deuterated derivatives (Majumdar+ 2014)Byte-by-byte Description of file: table2.dat   Bytes Format Units   Label     Explanations   1-  6  A6    ---     Species   Isomer   8-  9  I2    ---     N'        Upper N quantum number  11- 12  I2    ---     Ka'       Upper Ka quantum number  14- 15  I2    ---     Kc'       Upper Kc quantum number  17- 18  I2    ---     I'        ? Upper I quantum number (1)  20- 21  I2    ---     F'        ? Upper F quantum number (1)  23- 24  I2    ---     N         Lower N quantum number  26- 27  I2    ---     Ka        Lower Ka quantum number  29- 30  I2    ---     Kc        Lower Kc quantum number  32- 33  I2    ---     I         ? Lower I quantum number (1)  35- 36  I2    ---     F         ? Lower F quantum number (1)  39- 49  F11.4 MHz     Freq      Observed frequency  53- 57  F5.3  MHz     Unc       Experimental uncertainty  61- 67  F7.4  MHz     O-C       Observed minus calculated frequencies  71- 74  F4.2  ---     Weight    ? Relative weight (2)  78- 80  A3    ---     Ref       Reference (3)J/A+A/609/A121 https://cdsarc.unistra.fr/viz-bin/ReadMe/J/A+A/609/A121?format=html&tex=true2 di 3 15/09/2020, 17:21 • Contact© Université de Strasbourg/CNRSNote (1): Omitted in cases of unresolved hyperfine componentsNote (2): Given only for blended linesNote (3): References as follows:           (a) = Zaleski et al. (2013ApJ...765L..10Z)           (b) = Takeo et al. (1986, CPL, 123, 229 )           (c) = Takano et al. (1990, J. Mol. Spectr., 141, 13)           (d) = This workAcknowledgements:    Mattia Melosso, mattia.melosso2(at)unibo.it(End)                                        Patricia Vannier [CDS]  17-Oct-2017The document above follows the rules of the Standard Description for Astronomical Catalogues; from this documentation it is possible to generate f77 program to load files intoarrays or line by lineJ/A+A/609/A121 https://cdsarc.unistra.fr/viz-bin/ReadMe/J/A+A/609/A121?format=html&tex=true3 di 3 15/09/2020, 17:21

VizieR Online Data Catalog: Lab measurements for C-cyanomethanimine (Melosso+, 2018)

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VizieR Online Data Catalog: Lab measurements for C-cyanomethanimine (Melosso+, 2018)

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