J/A+A/578/A45 E-BOSS. II. Catalogue second release (Peri+, 2015)
E-BOSS: An Extensive stellar BOw Shock Survey. II. Catalogue second release.
Peri C.S., Benaglia P., Isequilla N.L.
<Astron. Astrophys., 578, A45-45 (2015)>
=2015A&A...578A..45P 2015A&A...578A..45P
ADC_Keywords: Stars, early-type ; Surveys
Keywords: catalogs - stars: early-type - infrared: ISM
Abstract:
Stellar bow shocks have been studied not only observationally, but
also theoretically since the late 1980s. Only a few catalogues of them
exist. The bow shocks show emission along all the electromagnetic
spectrum, but they are detected more easily in infrared wavelengths.
The release of new and high-quality infrared data eases the discovery
and subsequent study of new objects.
We search stellar bow-shock candidates associated with nearby runaway
stars, and gather them together with those found elsewhere, to enlarge
the list of the E-BOSS first release. We aim to characterize the
bow-shock candidates and provide a database suitable for statistical
studies. We investigate the low-frequency radio emission at the
position of the bow-shock features, that can contribute to further
studies of high-energy emission from these objects.
We considered samples from different literature sources and searched
for bow-shaped structures associated with stars in the Wide-field
Infrared Survey Explorer (WISE) images. We looked for each bow-shock
candidate on centimeter radio surveys.
We reunited 45 bow-shock candidates and generated composed WISE images
to show the emission in different infrared bands. Among them there are
new sources, previously studied objects, and bow shocks found
serendipitously. Five bow shocks show evidence of radio emission.
Stellar bow shocks constitute an active field with open questions and
enormous amounts of data to be analyzed. Future research at all
wavelengths databases, and use of instruments like Gaia, will provide
a more complete picture of these objects. For instance, infrared
spectral energy distributions can give information about physical
parameters of the bow shock matter. In addition, dedicated
high-sensitivity radio observations can help to understand the
radio-γ connection.
Description:
E-BOSS first release (r1, Peri et al., 2012A&A...538A.108P 2012A&A...538A.108P) was based
on two samples. Group 1 consisted of a set of sources taken from
Noriega-Crespo et al. (1997AJ....113..780N 1997AJ....113..780N) and Group 2 was a list
extracted from Tetzlaff et al. (2011MNRAS.410..190T 2011MNRAS.410..190T, Cat.
J/MNRAS/410/190). To build the present and second E-BOSS release (r2)
we used samples extended to other spectral types, sources with no
public WISE data at the moment of making E-BOSS r1, bow shocks from
the literature, and bow shocks found serendipitously.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
groups.dat 28 366 List of stars for groups 3-6 (tables 1-4)
table5.dat 100 45 Group 7: Serendipity and literature
table6.dat 125 45 List of the E-BOSS release 2 bow-shock candidates
(BSC) and corresponding stellar parameters
table7.dat 55 39 Parameters of the bow-shock candidates and
medium density
table8.dat 25 73 Total list of bow-shock candidates of E-BOSS
releases 1 and 2
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See also:
J/MNRAS/410/190 : Young runaway stars within 3kpc (Tetzlaff+, 2011)
Byte-by-byte Description of file: groups.dat
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Bytes Format Units Label Explanations
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1 I1 --- Group [3/6] Group number (1)
3- 14 A12 --- Name Star name (2)
15- 16 A2 --- n_Name [* b+] Note (3)
17 A1 --- f_Name [a] Flag (4)
19- 28 A10 --- SpType MK spectral type (5)
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Note (1): Group definition as follows:
3 = Tetzlaff WISE 2. Stars from E-BOSS r1 Group 2 without WISE observations
4 = Tetzlaff B3-B5. Stars with spectral types from B3 to B5
5 = GOSC. Maiz-Apellaniz et al. 2004 (J/ApJS/151/103)
6 = Stars extracted from Hoogerwerf et al. (2001A&A...365...49H 2001A&A...365...49H).
We removed sources contained in groups 1 to 5
Note (2): For group 5: HIP names for sources already analyzed on previous
groups (1, 2, and 3), HD names for sources not analyzed on any other group.
Note (3): Notes as follows:
b = bow-shock candidates
* = Analyzed on E-BOSS r1 (2012A&A...538A.108P 2012A&A...538A.108P) using MSX data
** = special cases, see Sect. 4.5
no clear bow-shock structures, and we give more details in Sect. 4.5
+ = The star HIP 99527 has two possible spectral types, B4Ieq and K2Ib;
we decided to select the first one
Note (4): a: HIP 17358 was already studied on E-BOSS r1 (2012A&A...538A.108P 2012A&A...538A.108P)
Note (5): For groups 3 and 4, spectral types taken from Tetzlaff et al.
(2011, Cat. J/MNRAS/410/190).
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [G7-]
4- 5 I2 --- ID [1/45] Star number within the group (1)
6- 7 A2 --- n_ID [* ] already analyzed or no clear bow-shock (2)
9- 20 A12 --- Name Star Name
22- 23 I2 h RAh Right ascension (J2000) (3)
25- 26 I2 min RAm Right ascension (J2000)
28- 32 F5.2 s RAs Right ascension (J2000)
35 A1 --- DE- Declination sign (J2000)
36- 37 I2 deg DEd Declination (J2000)
39- 40 I2 arcmin DEm Declination (J2000)
42- 46 F5.2 arcsec DEs Declination (J2000)
48- 51 A4 --- Ref References for sources from other works (4)
53- 56 A4 --- WISE Flag for WISE images (5)
58- 61 A4 --- --- [Fig. -]
63- 64 I2 --- Fig [5/11]? Figure number in the present work
66-105 A40 --- Com Relevant comment for each case
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Note (1): For G7 01 to 34 we looked for bow-shock candidates in WISE images
using sources from other works (in Ref column).
G7 39 to 45 were serendipitously discovered during the catalogue production
Note (2): Notes as follows:
* = already analyzed in other Groups (1 to 6) of E-BOSS r1 or r2
** = no clear bow-shock structures, and we give more details in Sect. 4.5
Note (3): Coordinates: for stars that produce the bow shock (whenever possible),
or BSC apex coordinates estimated by us (visually), where the star could not
be identified.
Note (4): References as follows:
A = Povich et al. (2008ApJ...689..242P 2008ApJ...689..242P)
B = Kobulnicky et al. (2010ApJ...710..549K 2010ApJ...710..549K)
C = Gvaramadze et al. (2011A&A...535A..29G 2011A&A...535A..29G)
D = Arnal et al. (2011A&A...532A...9A 2011A&A...532A...9A)
E = Kaper et al. (1997ApJ...475L..37K 1997ApJ...475L..37K)
F = Gvaramadze et al. (2011A&A...529A..14G 2011A&A...529A..14G)
G = Ankay et al. (2001A&A...370..170A 2001A&A...370..170A)
H = Gvaramadze et al. (2013MNRAS.430L..20G 2013MNRAS.430L..20G)
I = Gvaramadze et al. (2014MNRAS.437.2761G 2014MNRAS.437.2761G)
J = Gvaramadze & Bomans (2008A&A...490.1071G 2008A&A...490.1071G)
K = Liu et al. (2011ApJ...733L...2L 2011ApJ...733L...2L, Cat. J/ApJ/733/L2)
L = Magnier et al. (1999A&A...352..228M 1999A&A...352..228M, Cat. J/A+A/352/228)
M = Sahai et al. (2012ApJ...751...69S 2012ApJ...751...69S)
Note (5): Flags as follows:
Inc = bow-shock shape observed in WISE images
Inc? = bow-shock candicate (BSC) to be confirmed
. = emission excess in the region of bow-shock
? = doubtful cases, detailed in section Special cases
+ = not enough resolution to identify bow-shock shape in WISE images
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Name Star name
14 A1 --- n_Name [1] Velocity estimated from proper motion (1)
16- 18 A3 --- Group Group(s) number of the source (3-7)
20- 25 F6.2 deg GLON Galactic longitude
27- 32 F6.2 deg GLAT Galactic latitude
34- 56 A23 --- SpType MK spectral type (2)
58- 64 F7.2 pc Dist [175/7600]?=- Heliocentric distance
66- 70 F5.1 pc e_Dist [0.1/190]? rms uncertainty on Dist
71 A1 --- r_Dist [abz] Reference for Dist (3)
72 A1 --- f_Dist [h] h indicates distance derived from Hipparcos
parallaxes (van Leeuwen, 2007, I/311)
74- 77 I4 km/s Vinf [100/2900]?=- Wind terminal velocity
V∞ (4)
78 A1 --- f_Vinf [p] p indicates value adopted in Peri et al.
(2012A&A...538A.108P 2012A&A...538A.108P) for stars with same
spectral types
80- 83 F4.2 MMsun/yr dM/dt [0.03/3.3]?=- Mass loss rate (5)
86- 89 F4.1 km/s Vtg [13/57]?=- Tangential velocity (6)
91- 96 F6.2 km/s RV [-42/32]?=- Radial velocity (7)
98- 99 I2 km/s e_RV [2/15]? rms uncertainty on RV
101-106 F6.2 mas/yr pmRA [-35/11]?=- Proper motion along RA (*cosDE) (8)
107 A1 --- --- [/]
108-113 F6.2 mas/yr pmRA2 [-12/8]? Second proper motion along RA value,
114-119 F6.2 mas/yr pmDE [-11/15]?=- Proper motion along DE (8)
120 A1 --- --- [/]
121-125 F5.1 mas/yr pmDE2 [-12/19]? Second proper motion along DE value
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Note (1): 1: for HIP 44368, the tangential velocity is estimated through
proper motion values
Note (2): for B-type stars from Simbad; for O-type stars (whenever possible)
from GOS Catalog (Maiz-Apellaniz et al., 2004, Cat. J/ApJS/151/103),
otherwise from same reference as in Table 5.
Note (3): References as follows:
a = Megier et al. (2009, Cat. J/A+A/507/833)
b = Mason et al. (1998AJ....115..821M 1998AJ....115..821M),
z = from same references of Table 5
Note (4): inter or extrapolated from Table 3, Prinja et al.
(1990ApJ...361..607P 1990ApJ...361..607P).
Note (5): Mass loss rate in 106M☉/yr, inter or extrapolated from
Vink et al. (2001A&A...369..574V 2001A&A...369..574V).
Note (6): For sources of groups 3 and 4 from Tetzlaff et al. (2011,
Cat. J/MNRAS/410/190) except HIP 44368.
Note (7): for groups 3 to 6, from Kharchenko et al. (2007, Cat. J/AN/328/889);
for objects from Group 7, references as in Table 5, and Simbad for
SER 1, 3, 4, and 5.
Note (8): for groups 3 to 6, and K3 (HD 195229), from van Leeuwen (2007,
Cat. I/311); for G1 to G8 we show two values from Gvaramadze et al.
(2011A&A...535A..29G 2011A&A...535A..29G); for TYC 3159-6-1, BD-14 5040, and Star 1, reference as
in Table 5 (see errors for velocities and proper motions in references);
for SER 1, 3, 4, and 5, Simbad.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1 A1 --- d [d] d for stars with known distances
3- 14 A12 --- Name Star name
15 A1 --- n_Name [*] Star studied in r1 (1)
19- 23 F5.2 arcmin l1 [1/22] Angular length of bow-shock structure (2)
25- 28 F4.2 arcmin w1 [0.3/4] Angular width of bow-shock structure (2)
30- 32 F3.1 arcmin R1 [0.3/5] Angular distance of the bow-shock
structure (2)
35- 38 F4.2 pc l2 [0.09/10]? Length of the bow-shock structure (2)
in linear unit (2)
40- 43 F4.2 pc w2 [0.02/2]? Width of the bow-shock structure (2)
in linear unit (2)
45- 48 F4.2 pc R2 [0.05/2]? Distance of the bow-shock structure (2)
in linear unit (2)
50- 55 F6.2 cm-3 nISM [0.1/380]? Ambient density as derived in
Peri et al. 2012A&A...538A.108P 2012A&A...538A.108P; and
Wilkin 1996ApJ...459L..31W 1996ApJ...459L..31W
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Note (1): Note as follows:
* = Studied in E-BOSS r1 (Peri et al. 2012A&A...538A.108P 2012A&A...538A.108P)
only through MSX images
Note (2): The sizes were estimated from WISE band 4 (22um) images, and with
band 3 (12.1um) images when identification was not clear in band 4.
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- ID Source identification (EBNN)
6- 17 A12 --- Name Star name
20- 21 A2 --- Rel Release (r1 or r2)
23- 25 A3 --- Group Group(s) number
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References:
Peri et al., Paper I 2012A&A...538A.108P 2012A&A...538A.108P
(End) Patricia Vannier [CDS] 29-Jul-2015