J/ApJ/814/52 3600-24700Å deep X-shooter spectrum of HH 1 (Giannini+, 2015)
Solving the excitation and chemical abundances in shocks: the case of HH 1.
Giannini T., Antoniucci S., Nisini B., Bacciotti F., Podio L.
<Astrophys. J., 814, 52 (2015)>
=2015ApJ...814...52G 2015ApJ...814...52G (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics ; Spectroscopy ; Interstellar medium
Keywords: atomic data; Herbig-Haro objects; ISM: abundances; ISM: atoms;
ISM: individual; line: identification
Abstract:
We present deep spectroscopic (3600-24700Å) X-shooter observations
of the bright Herbig-Haro object HH 1, one of the best laboratories to
study the chemical and physical modifications caused by protostellar
shocks on the natal cloud. We observe atomic fine structure lines, HI
and HeI recombination lines and H2 ro-vibrational lines (more than
500 detections in total). Line emission was analyzed by means of
Non-local Thermal Equilibiurm codes to derive the electron temperature
and density, and for the first time we are able to accurately probe
different physical regimes behind a dissociative shock. We find a
temperature stratification in the range 4000K/80000K, and a
significant correlation between temperature and ionization energy. Two
density regimes are identified for the ionized gas, a more tenuous,
spatially broad component (density ∼103/cm3), and a more compact
component (density≥105/cm3) likely associated with the hottest
gas. A further neutral component is also evidenced, having a
temperature ≲10000K and a density >104/cm3. The gas fractional
ionization was estimated by solving the ionization equilibrium
equations of atoms detected in different ionization stages. We find
that neutral and fully ionized regions co-exist inside the shock.
Also, indications in favor of at least partially dissociative shock as
the main mechanism for molecular excitation are derived. Chemical
abundances are estimated for the majority of the detected species. On
average, abundances of non-refractory/refractory elements are lower
than solar of about 0.15/0.5dex. This indicates the presence of dust
inside the medium, with a depletion factor of iron of ∼40%.
Description:
A summary of the observations of HH 1 was already given in Paper I
(Giannini+, 2015ApJ...798...33G 2015ApJ...798...33G). We collected 7 X-shooter
observations (resolving power of 9900, 18200 and 7780 for the UVB
(3600-5900Å), VIS (5450-10200Å) and NIR arm (9900-24700Å))
of HH 1 (pointing: RAJ2000=05:36:20.27,DEJ2000=-06:45:04.84), in the
period November 1 2013-January 2 2014, each integrated 30min on-source.
Objects:
--------------------------------------------
RA (ICRS) DE Designation(s)
--------------------------------------------
05 36 20.2 -06 45 05 HH 1 = HH 1
--------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table5.dat 95 232 Atomic forbidden lines
table6.dat 83 66 Recombination lines
table7.dat 52 258 H2 lines
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See also:
VI/64 : Recombination line intensities for hydrogenic ions (Storey+ 1995)
J/A+A/524/A35 : Effective collision strengths of CrII (Wasson+, 2010)
J/ApJS/188/32 : Breit-Pauli transition probabilities for SII (Tayal+, 2010)
J/ApJ/711/1236 : Equivalent width of H2 from FUSE (Jensen+, 2010)
J/MNRAS/395/855 : Spectroscopy (310-1040nm) of HH 202 (Mesa-Delgado+, 2009)
J/A+A/481/123 : Near-IR IFU spectroscopy of HH99B (Giannini+, 2008)
J/A+A/474/941 : Spectroscopy of H2 towards HH91A (Gredel+, 2007)
J/A+A/469/1203 : IRON project LXIV (Melendez+, 2007)
J/A+A/420/763 : Electron impact excitation of NiII (Bautista+, 2004)
J/A+AS/141/297 : H2 total transition probability (Abgrall+, 2000)
J/A+AS/119/523 : IRON project XVIII. Fe III data (Zhang 1996)
J/A+AS/108/1 : IRON Project. V. O-like ions (Butler+, 1994)
J/A+AS/103/273 : IRON Project II. C-like ions (Lennon+ 1994)
http://www.pa.uky.edu/~peter/atomic/ : Atomic line list
http://www.nist.gov/pml/data/asd.cfm : NIST atomic spectra database
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- El Element
12- 13 I2 --- Z [6/28] Atomic number
15- 23 F9.3 0.1nm lambda [3726/22534.6] Wavelength in air; Angstroms
25- 26 I2 --- f_lambda [1/38]? Flag on lambda (1)
28- 35 A8 --- Ion Ion designation
37- 47 A11 --- Upper Upper level designation
49- 59 A11 --- Lower Lower level designation
61- 68 F8.2 cm-1 Eup [4628.6/43185.8] Upper level energy
70- 77 F8.2 cm-1 Elo [0/26830.6] Lower level energy
79- 85 F7.2 10-17mW/m2 Flux1 [0.6/1251] Line flux; 1e-17ergs/s/cm2 (2)
87- 91 F5.1 10-17mW/m2 Flux2 [0.6/207.2]? Second component, if present,
line flux (2)
93- 95 F3.1 10-17mW/m2 DelFlux [0.2/1.5] Uncertainty in total line flux
--------------------------------------------------------------------------------
Note (1): Flag as follows:
1 = Blended with [O II] 2Po3/2 - 2Do5/2;
2 = Blended with [O II] 2Po1/2 - 2Do5/2;
3 = Blended with [O II] 2Po3/2 - 2Do3/2;
4 = Blended with [O II] 2Po1/2 - 2Do3/2;
5 = Blended with [Fe II] b4P5/2 - a6D5/2;
6 = Blended with [Fe II] b4P5/2 - a6D3/2;
7 = Blended with [Fe III] 3G4 -5D4;
8 = Blended with [Fe II] a2F7/2 - a4P3/2;
9 = Blended with [Cr II] b4D7/2 - a6S5/2
and [Ni II] 2D5/2 - 2D5/2;
10 = Blended with [Cr II] b4D1/2 - a6S5/2
and [Ni II] 2D5/2 - 2D5/2;
11 = Blended with [Cr II] a4P5/2 - a6S5/2;
12 = Blended with [Cr II] a4P3/2 - a6S5/2;
13 = Blended with [Fe II] a4P5/2 - a6D1/2;
14 = Blended with [Fe II] b2P3/2 - a6D7/2;
15 = Blended with [Fe II] a4G9/2 - a6D7/2;
16 = Blended with [Fe II] a2F5/2 - a4F7/2;
17 = Blended with [Fe II] a4G5/2 - a6D3/2;
18 = Blended with [Fe II] a4G7/2 - a4F7/2;
19 = Blended with [Fe II] a4G11/2 - a4F9/2;
20 = Blended with [Fe II] b4F3/2 - a6D7/2;
21 = Blended with [Fe II] a6S5/2 - a6D5/2;
22 = Blended with He I 3D - 3Po;
23 = Blended with [O III] 1D_2 - 3P_1;
24 = Blended with [O III] 1D_2 - 3P_2;
25 = Blended with [Fe III] 3P4 - 5D1;
26 = Blended with [Ca II] 2D3/2 - 2S1/2;
27 = Blended with [Fe II] a4P3/2 - a6D5/2;
28 = Blended with [Fe II] a2G9/2 - a4F5/2;
29 = Blended with H2 3-0 S(13);
30 = Blended with [Cr II] a6D9/2 - a6S5/2;
31 = Blended with He I 3D & 3Po;
32 = Blended with [Fe II] b2H11/2 - a2H11/2 and H2 3-1 O(8);
33 = Blended with [Fe II] b2F5/2 - a4G7/2 and H2 3-1 O(8);
34 = Blended with [S II] 2Po3/2 - 4So3/2;
35 = Blended with [Fe II] a2D23/2 - a4F5/2;
36 = Blended with H2 7-5 Q(1);
37 = Blended with [Cr II] b4D1/2 - a6S5/2
and [Cr II] b4D7/2 - a6S5/2;
38 = Blended with H2 4-1 S(6).
Note (2): We do not report the flux of lines well detected both in the spectral
images and the 1-D spectrum but contaminated by image artifacts or
located in spectral segment with poor atmospheric transmission.
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Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Sp Species identifier (Helium I, Helium II or
Hydrogen)
11- 18 F8.2 0.1nm lam1 [3669.4/21655.3] Wavelength or
Lower wavelength range; Angstroms
19 A1 --- --- [-]
20- 27 F8.2 0.1nm lam2 ? Upper wavelength range; Angstroms
29 I1 --- f_lam1 [1/3]? Flag on lambda (1)
31- 38 A8 --- Upper Upper level designation
40- 47 A8 --- Lower Lower level designation
49- 57 F9.2 cm-1 Eup [97492.3/411478] Upper level energy
59- 67 F9.2 cm-1 Elo [82259.1/390142.4] Lower level energy
69- 73 F5.1 10-17mW/m2 Flux1 [0.8/939.6] Line flux; 1e-17 ergs/s/cm2
75- 79 F5.1 10-17mW/m2 Flux2 [2.9/259]? Second component, if present,
line flux
81- 83 F3.1 10-17mW/m2 DelFlux [0.2/1.1] Uncertainty in total line flux
--------------------------------------------------------------------------------
Note (1): Flag as follows:
1 = Blended with H2 7-5 S(2);
2 = Blended with [Fe II] b4F3/2 - a6D5/2;
3 = Blended with [Fe II] a2D25/2-a4D3/2.
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Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 I1 --- v [1/9] H2 v value
3- 10 F8.2 0.1nm lambda [7091.8/24748.7] Wavelength in air; Angstroms
12- 13 A2 --- f_lambda Flag on lambda (1)
15- 23 A9 --- Trans Transition
25- 32 F8.2 cm-1 Eup [6149.5/49194.6] Upper level energy
34- 42 F9.3 cm-1 Elo [0/42122.2] Lower level energy
44- 48 F5.1 10-17mW/m2 Flux [0.5/276]? Line flux; 1e-17ergs/s/cm2 (2)
50- 52 F3.1 10-17mW/m2 e_Flux [0.2/1.3]? Uncertainty in line flux
--------------------------------------------------------------------------------
Note (1): Flag as follows:
1 = Blended with H2 7-4 S(12);
2 = Blended with H2 3-1 S(6);
3 = Blended with [Fe II] b4D5/2 - a2P1/2;
4 = Blended with H2 6-3 S(7);
5 = Blended with H2 7-4 Q(3);
6 = Blended with H2 2-0 S(19);
7 = Blended with [FeII] b2F5/2 - a4G7/2
and [Fe II] b2H11/2 - a2H11/2;
8 = Blended with [Ni II] 2F7/2 - 2D3/2;
9 = Blended with H2 6-3 S(6);
10 = Blended with H2 4-2 S(6);
11 = Blended with H2 4-2 S(13);
12 = Blended with H2 5-3 S(7) and H2 5-3 S(11);
13 = Blended with H2 5-3 S(8);
14 = Blended with H2 5-3 S(10);
15 = Blended with H2 5-3 S(7) and H2 4-1 O(13);
16 = Blended with H2 5-3 S(11) and H2 4-1 O(13);
17 = Blended with H2 3-0 Q(12);
18 = Blended with H2 4-1 O(3);
19 = Blended with H2 2-0 S(15);
20 = Blended with H2 3-1 S(10);
21 = Blended with H I 14-4;
22 = Blended with [Co II] b3F4 - a5F4.
Note (2): We do not report the flux of lines well detected both in the spectral
images and the 1-D spectrum but contaminated by image artifacts or
located in spectral segment with poor atmospheric transmission.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 23-Feb-2016