J/A+A/664/A11       NIR spectroscopic survey of protostellar jets (Massi+, 2022)

NIR spectroscopic survey of protostellar jets in the star forming region IC 1396N. Massi F., Lopez R., Beltran M.T., Estalella R., Girart J.M. <Astron. Astrophys. 664, A11 (2022)> =2022A&A...664A..11M 2022A&A...664A..11M (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Infrared sources ; Spectra, infrared ; Photometry, narrow-band Keywords: ISM: jets and outflows - ISM: individual objects: IC1396N - stars: formation - infrared: ISM - techniques: spectroscopic Abstract: The bright-rimmed cloud IC 1396N, associated with an intermediate-mass star-forming region, hosts a number of CO, molecular hydrogen, and Herbig-Haro (HHs) outflows powered by a set of millimetre compact sources. The aim of this work is to characterise the kinematics and physical conditions of the H2 emission features spread throughout the IC 1396N region. The features appear as chains of knots with a jet-like morphology and trace different H2 outflows. We also obtain further information about (and an identification of) the driving sources. Low-resolution, long-slit near-infrared spectra were acquired with the NICS camera at the TNG telescope, using grisms KB (R∼1200), HK, and JH (R∼500). Several slit pointings and position angles were used throughout the IC 1396N region in order to sample a number of the H2 knots that were previously detected in deep H2 2.12um images. The knots exhibit rich ro-vibrational spectra of H2, consistent with shock-excited excitation, from which radial velocities and relevant physical conditions of the IC 1396N H2 outflows were derived. These also allowed estimating extinction ranges towards several features. [FeII] emission was only detected towards a few knots that also display unusually high H2 1-0 S(3)/S(1) flux ratios. The obtained radial velocities confirm that most of the outflows are close to the plane of the sky. Nearby knots in the same chain often display different radial velocities, both blue-shifted and red-shifted, which we interpret as due to ubiquitous jet precession in the driving sources or the development of oblique shocks. One of the chains (strand A, i.e. knots A1 to A15) appears as a set of features trailing a leading bow-shock structure consistent with the results of 3D magneto-hydrodynamical models. The sides of the leading bow shock (A15) exhibit different radial velocities. We discuss possible explanations. Our data cannot confirm whether strands A and B have both originated in the intermediate mass young stellar object [BGE2002] BIMA 2 because a simple model of a precessing jet cannot account for their locations. Near-infrared spectroscopy has confirmed that most of the H2 ro-vibrational emission in IC 1396N is shock-excited rather than uv-excited in photon-dominated regions. It has shown a complex kinematical structure in most strands of emitting knots as well. Description: Table 3 lists the fluxes of all the lines identified, knot by knot, in the bands HK and JH. For each knot, all line fluxes are normalised to the H2 1-0 S(1) ro-vibrational line flux in the HK band, and to the H2 1-0 S(7) ro-vibrational line flux in the JH band. If a flux error is marked by 9999, this indicates that the corresponding flux is an upper limit. If both flux and flux error are marked by 9999, this indicates that either the band does not cover the corresponding wavelength or the knot has not been observed through the corresponding grism. If a flux is marked by 8000, this indicates that line detection was impossible due to problems (usually bad pixels or noise due to the telluric correction). Table 4 lists the fluxes of all the lines identified, knot by knot, in the band of grism KB. For each knot, all line fluxes are normalised to the H2 1-0 S(1) ro-vibrational line flux. If a flux error is marked by 9999, this indicates that the corresponding flux is an upper limit. If a flux is marked by 8000, this indicates that line detection was impossible due to problems (usually bad pixels). Quoted uncertainties have been obtained by multiplying the r.m.s. measured outside the line by the FWHM of an unresolved line. Upper limits have been calculated as the r.m.s. times the expected FWHM (which is just instrumental) multiplied by 3. All line fluxes, excepted those of knots observed only in the JH band, can be calibrated using the fluxes provided in Table 5. Table 5 lists the H2 1-0 S(1) line fluxes for the knots with entries in Table 3 and 4 based on the narrow-band photometry (2.12 micron) by Beltran et al. (2009). We have updated the photometry to include feature unclassified in that paper, as well. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file list.dat 75 79 List of studied knots table3.dat 69 1399 Normalised line fluxes per knot in the HK and JH bands table4.dat 49 598 Normalised line fluxes per knot in the KB band table5.dat 19 49 Knot line fluxes in the H2 1-0 S(1) line -------------------------------------------------------------------------------- See also: J/A+A/504/97 : JHKs photometry of IC 1396N (Beltran+, 2009) Byte-by-byte Description of file: list.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 7 A7 --- ID Knot identification 11- 20 A10 ---- FileName1 First table name with data for the knot 22- 31 A10 ---- FileName2 Second table name with data for the knot 33- 42 A10 ---- FileName3 Third table name with data for the knot 45- 47 A3 --- Name Knot name or near knot name in Beltran et al. (2009, Cat. J/A+A/504/97) 52- 53 I2 h RAh ? Right ascension (J2000) for source in Beltran et al. (2009, Cat. J/A+A/504/97) 55- 56 I2 min RAm ? Right ascension (J2000) for source in Beltran et al. (2009, Cat. J/A+A/504/97) 58- 62 F5.2 s RAs ? Right ascension (J2000) for source in Beltran et al. (2009, Cat. J/A+A/504/97) 64 A1 --- DE- Declination sign (J2000) for source in Beltran et al. (2009, Cat. J/A+A/504/97) 65- 66 I2 deg DEd ? Declination (J2000) for source in Beltran et al. (2009, Cat. J/A+A/504/97) 68- 69 I2 arcmin DEm ? Declination (J2000) for source in Beltran et al. (2009, Cat. J/A+A/504/97) 71- 75 F5.2 arcsec DEs ? Declination (J2000) for source in Beltran et al. (2009, Cat. J/A+A/504/97) -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 2- 6 A5 --- ID Knot identification (1) 8- 11 A4 --- SP Emitting molecular or ionic species (2) 13 I1 --- Up [1/4] Upper vibrational level (H2) or flag for upper electronic level ([FeII]) (3) 15 I1 --- Low [0/4] Lower vibrational level (H2) or flag for lower electronic level ([FeII]) (3) 17 A1 --- DJ [0OQS] Difference between initial and final rotational level (H2) or 0 ([FeII]) (4) 19- 20 I2 --- J Final rotational level (H2) or 0 ([FeII]) 22- 27 F6.4 um lambda Transition wavelength (in vacuum) 29- 37 F9.4 --- FHK ?=9999 Normalised flux of lines in HK band (5) 39- 47 F9.4 --- e_FHK ?=9999 Error on normalised flux (5) 49- 57 F9.4 --- FJH ?=9999 Normalised flux of lines in JH band (6) 59- 67 F9.4 --- e_FJH ?=9999 Error on normalised flux (6) 69 A1 --- Flag Notes (7) -------------------------------------------------------------------------------- Note (1): Following the notation by Beltran et al. (2009, Cat. J/A+A/504/97). In case the first letter is lowercase: a,b,c,d indicate the frame where the knot spectrum was recorded (used when the same knots were observed with different slit settings); N and S as last letters indicate that the slit probably encompassed the northern or southern part of the knot. In a few cases, notably A15N and A15S, we checked that they are actually different knots and updated the photometry of Beltran et al. (2009, Cat. J/A+A/504/97) accordingly. Note (2): Species as follows: H2 = molecular hydrogen FeII = ionised iron Note (3): as for Fe+, forbidden lines ([FeII]) between levels, as follows: 1 = 3 d^6 (^5D) 4s (a^4D) J=7/2 2 = 3 d^7 (a^4F) J=9/2 3 = 3 d^6 (^5D) 4s (a^6D) J=7/2 4 = 3 d^6 (^5D) 4s (a^6D) J=9/2 Note (4): Jinitial - Jfinal = +2 (S), 0 (Q), -2 (O) Note (5): lines in the HK band normalised to the flux of H2 1-0 S(1) Note (6): lines in the JH band normalised to the flux of H2 1-0 S(7) Note (7): Notes as follows: c = when flux is not an upper limit, it flags the detection as certain p = when flux is not an upper limit, it flags the detection as possible e = values to be taken with caution due to heavy telluric absorption f = it may be merged with H2 5-3 S(5) at 1.3103 micron g = it may be merged with H2 4-2 S(3) at 1.2612 micron h = it may be merged with H2 4-2 S(4) at 1.2418 micron i = it may be merged with H2 3-1 S(6) at 1.1393 micron l = it may be merged with H2 3-1 S(11) at 1.1208 micron m = flux difficult to estimate due to nearby H2 lines, possible partial merging -------------------------------------------------------------------------------- Byte-by-byte Description of file: table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 2- 8 A7 --- ID Knot identification (1) 10- 11 A2 --- SP Emitting molecular or ionic species (2) 13 I1 --- Up [1/3] Upper vibrational level (H2) 15 I1 --- Low [0/2] Lower vibrational level (H2) 17 A1 --- DJ [S] Difference between initial and final rotational level (H2) (3) 19- 20 I2 --- J Final rotational level (H2) 22- 27 F6.4 um lambda Transition wavelength (in vacuum) 29- 37 F9.4 --- FKB ?=8000 Normalised flux of lines in KB band (4) 39- 47 F9.4 --- e_FKB ?=9999 Error on normalised flux (4) 49 A1 --- Flag Notes (5) -------------------------------------------------------------------------------- Note (1): Following the notation by Beltran et al. (2009, Cat. J/A+A/504/97). In case the first letter is "u", this indicates that the knot is unclassified in Beltran et al. (2009, Cat. J/A+A/504/97); in this case i) if the name of just one knot follows the "u", this is the nearest knot ii) if the names of two knots follow the "u", the unclassified knot lies between the two iii) if the name(s) of the knot(s) is(are) followed by N,S,E,W, this means that the unclassified knot lies North, South, etc. of the indicated knot(s). In case N,S,E,W follows the name of a classified knot, this indicates that the slit encompassed the northern, southern, etc. part of the knot. In a few cases, e. g. A15N and A15S, we checked that they are actually different knots and updated the photometry of Beltran et al. (2009, Cat. J/A+A/504/97) accordingly, as we have done for the "unclassified" knots. In case two classified knots are indicated, either the emitting area lies between the two or it was impossible to separate their contribution to the detected spectrum. A7p indicates that the emission comes from a plateau located near to A7, located to the south-east. A16 is a previously unclassified faint knot north-east of A15S. The photo-ionised strip is indicated as "pis". Note (2): Species as follows: H2: molecular hydrogen Note (3): Jinitial - Jfinal = +2 (S), 0 (Q), -2 (O) Note (4): normalised to the flux of H2 1-0 S(1) Note (5): Notes as follows: c = when flux is not an upper limit, it flags the detection as "certain" u = detection flagged as "uncertain" (only two cases) -------------------------------------------------------------------------------- Byte-by-byte Description of file: table5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 2- 8 A7 --- ID Knot identification (1) 10- 14 F5.2 aW/m2 F(H2) Flux measured in H2 filter (narrow-band filter centred on 2.12 micron) 16- 19 F4.2 aW/m2 e_F(H2) rms uncertainty on flux -------------------------------------------------------------------------------- Note (1): Following the notation by Beltran et al. (2009, Cat. J/A+A/504/97), as modified in table 3 and 4. -------------------------------------------------------------------------------- Acknowledgements: Fabrizio Massi, fabrizio.massi(at)inaf.it, INAF - Osservatorio Astrofisico di Arcetri, Italy References: Beltran et al., 2009A&A...504...97B 2009A&A...504...97B, Cat. J/A+a/504/A97 Beltran et al., 2012A&A...542L..26B 2012A&A...542L..26B, Close encounters of the protostellar kind in IC 1396N. Lopez et al., 2022A&A...661A.106L 2022A&A...661A.106L, Collision of protostellar jets in the star-forming region IC 1396N. Analysis of knot proper motions
(End) Fabrizio Mass [INAF, Italy], Patricia Vannier [CDS] 19-May-2022
The 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 into arrays or line by line