2018A&A...612A..12H


Query : 2018A&A...612A..12H

2018A&A...612A..12H - Astronomy and Astrophysics, volume 612A, 12-12 (2018/4-1)

Systematic search for very-high-energy gamma-ray emission from bow shocks of runaway stars.

HESS COLLABORATION, ABDALLA H., ABRAMOWSKI A., AHARONIAN F., AIT BENKHALI F., AKHPERJANIAN A.G., ANDERSSON T., ANGUNER E.O., ARAKAWA M., ARRIETA M., AUBERT P., BACKES M., BALZER A., BARNARD M., BECHERINI Y., BECKER TJUS J., BERGE D., BERNHARD S., BERNLOHR K., BLACKWELL R., BOTTCHER M., BOISSON C., BOLMONT J., BORDAS P., BREGEON J., BRUN F., BRUN P., BRYAN M., BUCHELE M., BULIK T., CAPASSO M., CARR J., CASANOVA S., CERRUTI M., CHAKRABORTY N., CHALME-CALVET R., CHAVES R.C.G., CHEN A., CHEVALIER J., CHRETIEN M., COFFARO M., COLAFRANCESCO S., COLOGNA G., CONDON B., CONRAD J., CUI Y., DAVIDS I.D., DECOCK J., DEGRANGE B., DEIL C., DEVIN J., DEWILT P., DIRSON L., DJANNATI-ATAI A., DOMAINKO W., DONATH A., DRURY L.O., DUTSON K., DYKS J., EDWARDS T., EGBERTS K., EGER P., ERNENWEIN J.-P., ESCHBACH S., FARNIER C., FEGAN S., FERNANDES M.V., FIASSON A., FONTAINE G., FORSTER A., FUNK S., FUSSLING M., GABICI S., GAJDUS M., GALLANT Y.A., GARRIGOUX T., GIAVITTO G., GIEBELS B., GLICENSTEIN J.F., GOTTSCHALL D., GOYAL A., GRONDIN M.-H., HAHN J., HAUPT M., HAWKES J., HEINZELMANN G., HENRI G., HERMANN G., HERVET O., HINTON J.A., HOFMANN W., HOISCHEN C., HOLLER M., HORNS D., IVASCENKO A., IWASAKI H., JACHOLKOWSKA A., JAMROZY M., JANIAK M., JANKOWSKY D., JANKOWSKY F., JINGO M., JOGLER T., JOUVIN L., JUNG-RICHARDT I., KASTENDIECK M.A., KATARZYNSKI K., KATSURAGAWA M., KATZ U., KERSZBERG D., KHANGULYAN D., KHELIFI B., KIEFFER M., KING J., KLEPSER S., KLOCHKOV D., KLUZNIAK W., KOLITZUS D., KOMIN N., KOSACK K., KRAKAU S., KRAUS M., KRUGER P.P., LAFFON H., LAMANNA G., LAU J., LEES J.-P., LEFAUCHEUR J., LEFRANC V., LEMIERE A., LEMOINE-GOUMARD M., LENAIN J.-P., LESER E., LOHSE T., LORENTZ M., LIU R., LOPEZ-COTO R., LYPOVA I., MARANDON V., MARCOWITH A., MARIAUD C., MARX R., MAURIN G., MAXTED N., MAYER M., MEINTJES P.J., MEYER M., MITCHELL A.M.W., MODERSKI R., MOHAMED M., MOHRMANN L., MORA K., MOULIN E., MURACH T., NAKASHIMA S., DE NAUROIS M., NIEDERWANGER F., NIEMIEC J., OAKES L., O'BRIEN P., ODAKA H., OTTL S., OHM S., OSTROWSKI M., OYA I., PADOVANI M., PANTER M., PARSONS R.D., PEKEUR N.W., PELLETIER G., PERENNES C., PETRUCCI P.-O., PEYAUD B., PIEL Q., PITA S., POON H., PROKHOROV D., PROKOPH H., PUHLHOFER G., PUNCH M., QUIRRENBACH A., RAAB S., REIMER A., REIMER O., RENAUD M., DE LOS REYES R., RICHTER S., RIEGER F., ROMOLI C., ROWELL G., RUDAK B., RULTEN C.B., SAHAKIAN V., SAITO S., SALEK D., SANCHEZ D.A., SANTANGELO A., SASAKI M., SCHLICKEISER R., SCHUSSLER F., SCHULZ A., SCHWANKE U., SCHWEMMER S., SEGLAR-ARROYO M., SETTIMO M., SEYFFERT A.S., SHAFI N., SHILON I., SIMONI R., SOL H., SPANIER F., SPENGLER G., SPIES F., STAWARZ L., STEENKAMP R., STEGMANN C., STYCZ K., SUSHCH I., TAKAHASHI T., TAVERNET J.-P., TAVERNIER T., TAYLOR A.M., TERRIER R., TIBALDO L., TIZIANI D., TLUCZYKONT M., TRICHARD C., TSUJI N., TUFFS R., UCHIYAMA Y., VAN DER WALT D.J., VAN ELDIK C., VAN RENSBURG C., VAN SOELEN B., VASILEIADIS G., VEH J., VENTER C., VIANA A., VINCENT P., VINK J., VOISIN F., VOLK H.J., VUILLAUME T., WADIASINGH Z., WAGNER S.J., WAGNER P., WAGNER R.M., WHITE R., WIERZCHOLSKA A., WILLMANN P., WORNLEIN A., WOUTERS D., YANG R., ZABALZA V., ZABOROV D., ZACHARIAS M., ZANIN R., ZDZIARSKI A.A., ZECH A., ZEFI F., ZIEGLER A. and ZYWUCKA N.

Abstract (from CDS):


Context. Runaway stars form bow shocks by ploughing through the interstellar medium at supersonic speeds and are promising sources of non-thermal emission of photons. One of these objects has been found to emit non-thermal radiation in the radio band. This triggered the development of theoretical models predicting non-thermal photons from radio up to very-high-energy (VHE, E≥0.1TeV) gamma rays. Subsequently, one bow shock was also detected in X-ray observations. However, the data did not allow discrimination between a hot thermal and a non-thermal origin. Further observations of different candidates at X-ray energies showed no evidence for emission at the position of the bow shocks either. A systematic search in the Fermi-LAT energy regime resulted in flux upper limits for 27 candidates listed in the E-BOSS catalogue.
Aims. Here we perform the first systematic search for VHE gamma-ray emission from bow shocks of runaway stars.
Methods. Using all available archival H.E.S.S. data we search for very-high-energy gamma-ray emission at the positions of bow shock candidates listed in the second E-BOSS catalogue release. Out of the 73 bow shock candidates in this catalogue, 32 have been observed with H.E.S.S.
Results. None of the observed 32 bow shock candidates in this population study show significant emission in the H.E.S.S. energy range. Therefore, flux upper limits are calculated in five energy bins and the fraction of the kinetic wind power that is converted into VHE gamma rays is constrained.
Conclusions. Emission from stellar bow shocks is not detected in the energy range between 0.14 and 18TeV. The resulting upper limits constrain the level of VHE gamma-ray emission from these objects down to 0.1-1% of the kinetic wind energy.

Abstract Copyright: © ESO 2018

Journal keyword(s): radiation mechanisms: non-thermal - gamma rays: ISM - stars: early-type - gamma rays: stars

Simbad objects: 35

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Number of rows : 35
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 V* AE Aur Or* 05 16 18.1489437436 +34 18 44.347016027 5.48 6.18 5.96     O9.5V 535 1
2 * ups Ori V* 05 31 55.8601879 -07 18 05.537157 3.30 4.36 4.63 4.75 5.01 O9.7V 389 0
3 HD 48099 Be* 06 41 59.2307767004 +06 20 43.538696992 5.38 6.32 6.37 6.30 6.35 O5V((f))z+O9:V 283 0
4 HD 64315 Em* 07 52 20.2841727949 -26 25 46.683038109 8.76 9.49 9.24 9.63 8.86 O5.5Vz+O7V 107 1
5 V* GP Vel HXB 09 02 06.8610736194 -40 33 16.896402010 6.85 7.37 6.87 6.31 6.05 B0.5Ia 1402 0
6 SSTGLMC G284.0764-00.4322 * 10 22 23.0517387585 -57 44 28.085738320           O6V(~)~ 8 0
7 2MASS J10240306-5748356 * 10 24 03.063 -57 48 35.68           O9V 6 0
8 GUM 29 HII 10 24 14.6 -57 46 58           ~ 196 0
9 UCAC2 6537809 Em* 10 24 39.198 -57 45 21.15       14.2   OB 10 0
10 2MASS J11171292-6120085 * 11 17 12.9269039826 -61 20 08.573375718           O6V 5 0
11 HD 130298 Em* 14 49 33.7650159274 -56 25 38.473190977 9.14 10.06 9.83 9.65   O6.5III(n)(f) 52 0
12 HD 136003 * 15 20 42.8125886775 -56 07 57.440274246 6.47 7.00 6.79 7.68   B1Iab/b 47 0
13 * zet Oph Be* 16 37 09.5390545 -10 34 01.529471 1.73 2.58 2.56 2.46 2.50 O9.2IVnn 1758 2
14 TYC 7370-460-1 * 17 18 15.4062020431 -34 00 06.221222446   13.24 11.79     O6V((f))+O8V 9 0
15 2MASS J17220342-3414241 * 17 22 03.4358569663 -34 14 24.037459788           O5.5 5 0
16 GEN# +6.20114034 * 17 22 05.6184455944 -35 39 55.458656896   14.86 13.13     O8/B0III/V 7 0
17 2MASS J17225002-3403223 * 17 22 50.0218664120 -34 03 22.348331160           B0V 4 0
18 CXOU J172405.6-340710 * 17 24 05.6222300226 -34 07 09.509087526           ~ 5 0
19 2MASS J17271123-3414349 * 17 27 11.2377753495 -34 14 35.093006672           O7.5 6 0
20 2MASS J17271253-3330399 * 17 27 12.5311361487 -33 30 39.953291630           B0V 3 0
21 HD 319881 * 17 28 21.6707964150 -34 32 30.425692132 11.14 11.21 10.11 10.00   O6Vn 18 0
22 HD 161056 * 17 43 47.0220911640 -07 04 46.590611461 6.26 6.68 6.32 5.94 5.67 B3II/III 169 0
23 HD 165319 * 18 05 58.8360539028 -14 11 52.998719141 8.15 8.63 8.04 7.50 7.00 O9.7Ib 69 1
24 UCAC2 27149134 * 18 15 23.9660633346 -13 19 35.839053976           ~ 4 0
25 NGC 6618 258 Y*O 18 20 22.6996927707 -16 08 34.169784772 15.03 14.99 13.69     O8.5Vz 30 0
26 NGC 6618 326 Y*O 18 20 25.8679599700 -16 08 32.401696347 16.39 15.87 14.20     ~ 33 0
27 2MASS J18202666-1607088 Y*O 18 20 26.6651975848 -16 07 08.710009906     17.5     B2V 9 0
28 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1530 0
29 BD-14 5040 * 18 25 38.9004768858 -14 45 05.709498433   11.52 10.54 10.31   O5.5V(n)((f)) 25 0
30 V* V1182 Aql SB* 18 55 23.1253977999 +09 20 48.087039876 8.73 9.10 8.64     O7V(n)((f))z+B 109 0
31 4U 1907+09 HXB 19 09 37.9 +09 49 49   19.41 16.35 14.40 12.53 O8.5Iab 313 1
32 HD 227018 * 19 59 49.1027196111 +35 18 33.548528123 8.75 9.35 9.00     O6.5V((f))z 95 0
33 HD 195592 s*b 20 30 34.9690436039 +44 18 54.858025184 7.75 7.95 7.08 6.29 5.60 O9.7Ia 200 1
34 PSR J2030+4415 Psr 20 30 51.396 +44 15 38.73           ~ 43 0
35 BD+43 3654 s*b 20 33 36.0795380204 +43 59 07.362541702   11.24 10.06     O4If 52 0

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2021.10.27-22:54:16

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