2004ApJ...613..374A


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.25CET07:32:15

2004ApJ...613..374A - Astrophys. J., 613, 374-380 (2004/September-3)

A mid-infrared survey of L1641N with ISOCAM.

ALI B. and NORIEGA-CRESPO A.

Abstract (from CDS):

We present the results from our analysis of the Infrared Space Observatory (ISO) data on the L1641N outflow region located in the Orion A molecular cloud. The data were obtained with the array camera (ISOCAM) using two broadband filters, LW2 (6.7 µm) and LW3 (14 µm), and the narrowband circular variable filter (CVF), which provides low-resolution (R=λ/δλ∼40) spectra in the 5-17 µm region. We detect a total of 34 sources in the 7'.65x8'.40 region covered by the broadband filters. Four of these sources have no reported detection in previous studies of the region. The CVF data are available for only the central 3'.2x3'.2 portion of the total region, providing spectra for the brightest seven sources in that region. We find that the source previously identified as the near-IR counterpart to the IRAS-detected point source (IRAS 05338-0624) is not the brightest source in the wavelength region of the IRAS 12 µm filter. We find instead that a nearby object (within the beam of IRAS and not detected at near-IR wavelengths) outshines all other sources in the area by a factor of ∼2. Despite its brightness, we conclude that this second object is unlikely to be the source detected by IRAS because that would imply a positional error of ∼1' in the IRAS position. However, we also consider it unlikely that IRAS would not have spatially resolved and detected the second source. This implies that the second source must have brightened by at least 200 mJy in the decade between IRAS and ISO observations. A comparison of the near-IR (J-H vs. H-Ks) and mid-IR (H-Ksvs. [6.7µm]-[14µm]) color-color plots shows that while at near-IR wavelengths only four of the sources show evidence for emission above the values predicted from photospheric emission alone (hereafter referred to as excess emission), at least 85% of all sources show evidence for excess emission at mid-IR wavelengths. This result supports similar conclusions from L-band surveys. The CVF spectra suggest a range of evolutionary status in the program stars ranging from embedded young stellar objects to young disks. When combined with optical and near-IR age estimates, these results show active current star formation in the region that has been ongoing for at least 2 Myr.

Abstract Copyright:

Journal keyword(s): Infrared: ISM - ISM: Clouds - ISM: Individual: Alphanumeric: L1641N - Stars: Formation

Nomenclature: Fig.2, Table 2: [AN2004] NN (Nos 1-34).

Simbad objects: 39

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Number of rows : 39

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 M 42 HII 05 35 17.3 -05 23 28           ~ 3756 0
2 V* V822 Ori Or* 05 36 05.1622455181 -06 25 25.384029726     15.526   13.331 M1.5 23 0
3 BD-06 1250 Y*O 05 36 06.0442950478 -06 19 38.907293436   10.53 9.95 9.64   ~ 30 0
4 BD-06 1251 Y*O 05 36 06.8602924127 -06 23 35.296898707   11.25 10.80     F5.0 15 0
5 [RHS2000] 1-1530 Y*O 05 36 06.9360905226 -06 18 53.386479256     16.261   13.188 M4.5 10 0
6 V* V2645 Ori Or* 05 36 08.3337946888 -06 24 37.830278008           M5.5 15 0
7 V* V825 Ori Or* 05 36 09.4919673185 -06 18 36.365734891     15.192   13.061 M2 20 0
8 Parenago 2354 Y*O 05 36 10.4378069078 -06 20 01.538262960   15.16 14.244   12.782 K3 16 0
9 ESO-HA 1453 Y*O 05 36 11.4651957678 -06 22 22.127137557     19.604   15.646 K7 16 0
10 V* V2651 Ori Or* 05 36 12.6071606279 -06 23 39.554032988     17.931   14.562 M5 18 0
11 [HD93] 7 Y*O 05 36 12.968 -06 23 32.97     17.113   13.714 M2.5 13 0
12 [AN2004] 24 IR 05 36 14.48 -06 21 05.5           ~ 1 0
13 Parenago 2374 *iN 05 36 15.2289065819 -06 23 55.671836165   11.45 11.09 10.57   ~ 25 0
14 NAME LDN 1641 North HII 05 36 17.6 -06 22 10           ~ 216 0
15 2MASS J05361764-0622493 Y*O 05 36 17.65 -06 22 49.4           ~ 6 0
16 V* V832 Ori Or* 05 36 18.4801437124 -06 20 38.756236307     14.52   13.495 M0 30 0
17 [AN2004] 18 IR 05 36 18.8 -06 22 10           ~ 3 0
18 [AN2004] 20 IR 05 36 18.94 -06 22 56.7           ~ 1 0
19 V* V2660 Ori Or* 05 36 19.3844811108 -06 25 51.236456955     18.797   15.214 M5 16 0
20 [CTS93] N 7 IR 05 36 20.3 -06 21 47           ~ 2 0
21 V* V2667 Ori Or* 05 36 20.50080 -06 23 22.1532           ~ 8 0
22 [HD93] 20 Y*O 05 36 21.0663228802 -06 21 53.538212515           ~ 13 0
23 SDSS J053621.18-062331.2 Y*O 05 36 21.18 -06 23 31.1           ~ 5 0
24 V* V2670 Ori Or* 05 36 21.5715271516 -06 22 52.516641645     21.786   19.309 M0.5 16 0
25 V* V582 Ori Or* 05 36 21.83832 -06 26 02.0364     16.775   14.236 M0 22 0
26 2MASS J05362187-0623299 Y*O 05 36 21.8788825072 -06 23 29.917121328           M1 23 0
27 V* V2672 Ori Or* 05 36 22.4692541771 -06 23 44.771426068     21.277   17.052 M0.5 15 0
28 [AN2004] 17 Y*O 05 36 22.63 -06 21 27.6           ~ 6 0
29 [HD93] 30 Y*O 05 36 23.60 -06 24 51.4           ~ 10 0
30 V* V2674 Ori Or* 05 36 23.7809072971 -06 23 11.236186825     17.5     ~ 15 0
31 V* V2675 Ori Or* 05 36 24.0184878170 -06 25 26.994080636           ~ 12 0
32 V* V2676 Ori Or* 05 36 24.4808205585 -06 22 23.301507969     19.604   15.429 M4 18 0
33 HOPS 178 Y*O 05 36 24.61 -06 22 41.3           ~ 17 0
34 [AN2004] 4 Y*O 05 36 25.867 -06 24 58.73           ~ 11 0
35 V* V2681 Ori Or* 05 36 27.7165748230 -06 23 12.252636968     17.542   13.983 M5 21 0
36 [AN2004] 2 IR 05 36 30.10 -06 23 09.9           ~ 1 0
37 V* BD Ori Or* 05 36 32.3822161175 -06 19 19.821558239   13.8 13.30   12.173 G8 37 0
38 [AN2004] 19 IR 05 36 37.08 -06 18 53.0           ~ 1 0
39 NAME Ori A MoC 05 38 -07.1           ~ 2704 0

    Equat.    Gal    SGal    Ecl

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2020.11.25-07:32:15

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