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Hier Ist Wahrhaftig Ein Loch Im Himmel-The NGC 1999 Dark Globule Is Not

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Hier Ist Wahrhaftig Ein Loch Im Himmel-The NGC 1999 Dark Globule Is Not Astronomy & Astrophysics manuscript no. 14612 c ESO 2018 October 4, 2018 Letter to the Editor Hier ist wahrhaftig ein Loch im Himmel ⋆ ⋆⋆ The NGC1999 dark globule is not a globule T. Stanke1, A. M. Stutz2,3, J. J. Tobin4, B. Ali5, S. T. Megeath6, O. Krause2, H. Linz2, L. Allen7, E. Bergin4, N. Calvet4, J. Di Francesco8,9, W. J. Fischer6, E. Furlan10, L. Hartmann4, T. Henning2, P. Manoj11, S. Maret12, J. Muzerolle13, P. C. Myers14, D. Neufeld15, M. Osorio16, K. Pontoppidan17, C. A. Poteet6, D. M. Watson11, and T. Wilson1 1 ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching bei M¨unchen, Germany; e-mail: [email protected] 2 Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl 17, D-69117 Heidelberg, Germany 3 Department of Astronomy and Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA 4 Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA 5 NASA Herschel Science Center, California Institute of Technology, 770 South Wilson Ave, Pasadena, CA91125, USA 6 Department of Physics and Astronomy, University of Toledo, 2801 West Bancroft Street, Toledo, OH 43606, USA 7 National Optical Astronomy Observatory, 950 N. Cherry Ave., Tucson, AZ 85719, USA 8 Department of Physics and Astronomy, University of Victoria, P.O. Box 355, STN CSC, Victoria BC, V8W 3P6, Canada 9 National Research Council Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria BC, V9E 2E7, Canada 10 JPL, California Institute of Technology, Mail Stop 264767, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 11 Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA 12 Laboratoire d’Astrophysique de Grenoble, Universit´eJoseph Fourier, CNRS, UMR 571, BP 53, F-38041 Grenoble, France 13 Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA 14 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 15 Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA 16 Instituto de Astrofisica de Andalucia, CSIC, Camino Bajo de Huetor 50, E-18008, Granada, Spain 17 Division of Geological and Planetary Sciences 150-21, California Institute of Technology, Pasadena, CA 91125, USA ABSTRACT The NGC 1999 reflection nebula features a dark patch with a size of ∼10,000 AU, which has been interpreted as a small, dense foreground globule and possible site of imminent star formation. We present Herschel PACS far-infrared 70 and 160 µm maps, which reveal a flux deficit at the location of the globule. We estimate the globule mass needed to produce such an absorption feature to be a few tenths to a few M⊙. Inspired by this Herschel observation, we obtained APEX LABOCA and SABOCA submillimeter continuum maps, and Magellan PANIC near–infrared images of the region. We do not detect a submillimer source at the location of −2 the Herschel flux decrement; furthermore our observations place an upper limit on the mass of the globule of ∼2.4·10 M⊙. Indeed, the submillimeter maps appear to show a flux depression as well. Furthermore, the near–infrared images detect faint background stars that are less affected by extinction inside the dark patch than in its surroundings. We suggest that the dark patch is in fact a hole or cavity in the material producing the NGC 1999 reflection nebula, excavated by protostellar jets from the V 380 Ori multiple system. Key words. globules – ISM: individual (NGC 1999) – ISM: jets and outflows – infrared: ISM – (ISM:) dust, extinction 1. Introduction dust content absorbs the light of background stars. Dark clouds, ranging in mass and size from giant molecular clouds (GMCs) In the year 1774 C.E. Sir Friedrich Wilhelm Herschel first no- to tiny globules, are the sites of star formation in our Galaxy. ticed patches of sky in the constellation Scorpio that were devoid NGC1999 is a small reflection nebula in the LDN1641 arXiv:1005.2202v1 [astro-ph.GA] 12 May 2010 of stars. Unable to find even the faintest star in these regions, his portion of the OrionA GMC, located in a small group of 22 sister Caroline reported him to exclaim: “Hier ist wahrhaftig ein pre–main sequence stars and protostars, including the driving Loch im Himmel!” (“Truly there is a hole in the sky here!”). source of the prototypical Herbig–Haro objects HH1 and HH2 These dark areas are now known to be due to obscuring mate- (Megeath et al., in prep.). It is illuminated by the HerbigAe/Be rial (e.g., Barnard et al. 1927): clouds of molecular gas, whose star V 380 Ori, a multiple system with a circumsystem disk where the primary is a 100L⊙ B9 star exhibiting strong emis- ⋆ Herschel is an ESA space observatory with science instruments sion lines (e.g., Leinert et al. 1997; Hillenbrandet al. 1992; provided by European-led Principal Investigator consortia and with im- Alecian et al. 2009). NGC1999 features a compact (20–30′′) portant participation from NASA dark patch (see Fig. 1), which is described in the literature as ⋆⋆ This publication includes data acquired with the Atacama Pathfinder Experiment (APEX; proposal E-082.F-9807 and E-284.C- a dark globule and potential site of star formation (e.g., Herbig 5015). APEX is a collaboration between the Max-Planck-Institut f¨ur 1946, 1960; Warren-Smith et al. 1980), but which has neverbeen Radioastronomie, the European Southern Observatory, and the Onsala studied in greater detail before. Space Observatory. This paper includes data gathered with the 6.5 meter We report here the serendipitous and surprising detection Magellan Telescopes located at Las Campanas Observatory, Chile. with PACS of a 70 and 160 µm flux decrement at the location 2 T. Stanke et al.: Hier ist wahrhaftig ein Loch im Himmel NGC 1999 dark region HH35 V 380 Ori HH147 IRS HH1 HH1/2 VLA1 HH2 Fig. 2. NGC 1999/HH1/2 region as seen with Herschel PACS 0.6 pc 10,000 AU at 160 µm (left, the box marks the region shown in Fig.3), and APEX SABOCA at 350 µm (right, smoothed to 10′′ resolution), Fig. 1. NGC1999 and HH1/2 region (DSS, left) and HST all displayed with a logarithmic color stretch. F450W/F555W/F675W true color image of the NGC1999 dark patch. preserve the extended emission we estimated the sky and the cor- of NGC1999. The maps show a dark patch against the nebu- related signal drifts observed in PACS readouts (Sauvage et al. lous far–IR emission that closely resembles the dark patch seen 2010). To determine the baselines, we removed pixel–to–pixel at visible wavelengths. The MSX, ISO, and Spitzer space tele- electronic offsets using the median of the entire time stream, scopes have detected clouds in absorption at mid–IR (5-30 µm) then calculated the median for each frame/readout. The median wavelengths against the diffuse IR background of the Galaxy values were divided into 500 readout bins, and we took the min- (e.g., Bacmann et al. 2000; Stutz et al. 2008; Tobin et al. 2010; imum value for each bin. This approach preserves the extended Stutzetal. 2009a), in a few cases even at 70 µm (Stutz et al. emission at all spatial scales, but does not remove 1/f noise. The 2009b). However, the detection of the NGC1999 globule by final mosaic was created using the ”photProject” routine. PACS would be the first detection of a dark globule in absorp- Method2: Optimal mapping with MADmap2 to remove the tion at 160 µm. At wavelengths ≥ 160 µm, cold globules are nor- bolometer 1/f noise from the pixel time–line. The initial pro- mally detected through the emission from cold (10–30K) dust. cessing is the same as for Method1. However, instead of ’phot- Furthermore, absorption at these wavelengths requires extinc- Project’, MADmap is used to determine an optimal solution for tions in excess of 100 AV . each sky pixel. This method preserves extended emission and Motivated by the possible discovery of a 160 µm dark cloud, removes the 1/f noise, at the price of a reduced sensitivity. we obtained follow–up ground based submillimeter and near–IR (extinction) observations towards the globule. We did not de- tect the column density or mass of cold dust necessary to pro- 2.2. Other data duce such an absorption feature in the far–IR. We therefore con- APEX SABOCA and LABOCA — We obtained submillimeter clude that the dark globule is actually a cavity in the NGC1999 continuum maps using LABOCA and SABOCA on APEX. cloud carved by outflows from the V380Ori system. Thus, the LABOCA (Siringo et al. 2009) is a ∼250 bolometer array op- Herschel telescope has discovered what truly is a hole in the sky. erating at 870 µm, with a spatial resolution of 19′′. Observations were done on 2009 November 29 and 30 in fair conditions, 2. Observations and processing with precipitable water vapour (PWV) values around 1mm (τzenith,870 ∼ 0.26). We used a combination of spiral and straight 2.1. Herschel PACS observations on–the–fly scans in order to recover extended emission. Data reduction was done with the BOA software (Schuller et al., in NGC1999 was observed with Herschel (Pilbratt et al. 2010) prep.) following standard procedures, including iterative source with the PACS instrument (Poglitsch et al. 2010) at 70 modeling. SABOCA (Siringo et al. 2010) is a 37 bolometer ar- and 160 µm on 2009 October 9 (OBSIDs 1342185551 and ray operating at 350 µm, with a resolution of 7′′. 8. Data were 1342185552) as part of the Science Demonstration Phase ob- taken on 2009 December 1st and 3rd (NGC1999) and on 2008 servations of the Herschel Orion Protostar Survey (HOPS; P.I.
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