Hier ist wahrhaftig ein Loch im Himmel

Stanke, T.; Stutz, Amelia M.; Tobin, John J.; Ali, B.; Megeath, S. Thomas; Krause, O.; Linz, H.; Allen, Lori; Bergin, Edwin A.; Calvet, Nuria; Francesco, James Di; Fischer, William J.; Furlan, Elise; Hartmann, L.; Henning, Th.; Manoj, P.; Maret, S.; Muzerolle, James; Myers, Philip C.; Neufeld, David A.; Osorio, M. R. Zapatero; Pontoppidan, K. M.; Poteet, C. A.; Watson, D. M.; Wilson, Thomas L.

doi:10.1051/0004-6361/201014612

Cited by 26 publications

(32 citation statements)

References 21 publications

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“…The HOPS program was a far-IR survey of Spitzer identified protostars in the Orion molecular clouds. The HOPS team obtained and analyzed Herschel/PACS photometry of 330 protostars and PACS spectra of 36 protostars (Fischer et al 2010(Fischer et al , 2013Stanke et al 2010;Manoj et al 2013;Stutz et al 2013;Furlan et al 2016;Gonzalez-Garcia et al 2016). A detailed analysis of the far-IR spectra of the 21 brightest sources in the HOPS spectroscopy sample were presented in Manoj et al (2013).…”

Section: The Samplementioning

confidence: 99%

The Evolution of Far-Infrared Co Emission From Protostars

Manoj

Green

Megeath

et al. 2016

ApJ

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We investigate the evolution of far-IR CO emission from protostars observed with Herschel/PACS for 50 sources from the combined sample of HOPS and DIGIT Herschel key programs. From the uniformly sampled spectral energy distributions, whose peaks are well sampled, we computed the L bol , T bol ,and L L bol smm for these sources to search for correlations between far-IR CO emission and protostellar properties. We find a strong and tight correlation between far-IR CO luminosity (L CO fir ) and the bolometric luminosity (L bol ) of the protostars with µ L L CO fir bol 0.7 . We, however, do not find a strong correlation between L CO fir and protostellar evolutionary indicators, T bol and L L bol smm . FIRCO emission from protostars traces the currently shocked gas by jets/outflows, and far-IR CO luminosity, L CO fir , is proportional to the instantaneous mass-loss rate,Ṁ out . The correlation between L CO fir and L bol , then, is indicative of instantaneousṀ out tracking instantaneousṀ acc . The lack of acorrelation between L CO fir and evolutionary indicators T bol and L L bol smm suggests thatṀ out and, therefore,Ṁ acc do not show any clear evolutionary trend. These results are consistent with mass accretion/ejection in protostars being episodic. Taken together with the previous finding that the time-averaged mass-ejection/accretion rate declines during the protostellar phase, our results suggest that the instantaneous accretion/ejection rate of protostars is highly time variable and episodic, but the amplitude and/or frequency of this variability decreases with time such that the timeaveraged accretion/ejection rate declines with system age.

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Section: The Samplementioning

confidence: 99%

The Evolution of Far-Infrared Co Emission From Protostars

Manoj

Green

Megeath

et al. 2016

ApJ

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“…FIR 4 was also detected at 37.1 μm using FORCAST on SOFIA (source SOF 3 of Adams et al 2012). As part of HOPS, a Herschel open-time key program (e.g., Fischer et al 2010;Stanke et al 2010;Stutz et al 2013;Manoj et al 2013;W. J. Fischer et al 2014, in preparation;B.…”

Section: Data Overviewmentioning

confidence: 99%

On the Nature of the Deeply Embedded Protostar Omc-2 Fir 4

Furlan

Megeath

Osorio

et al. 2014

ApJ

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We use mid-infrared to submillimeter data from the Spitzer, Herschel, and Atacama Pathfinder Experiment telescopes to study the bright submillimeter source OMC-2 FIR 4. We find a point source at 8, 24, and 70 μm, and a compact, but extended source at 160, 350, and 870 μm. The peak of the emission from 8 to 70 μm, attributed to the protostar associated with FIR 4, is displaced relative to the peak of the extended emission; the latter represents the large molecular core the protostar is embedded within. We determine that the protostar has a bolometric luminosity of 37 L , although including more extended emission surrounding the point source raises this value to 86 L . Radiative transfer models of the protostellar system fit the observed spectral energy distribution well and yield a total luminosity of most likely less than 100 L . Our models suggest that the bolometric luminosity of the protostar could be as low as 12-14 L , while the luminosity of the colder (∼20 K) extended core could be around 100 L , with a mass of about 27 M . Our derived luminosities for the protostar OMC-2 FIR 4 are in direct contradiction with previous claims of a total luminosity of 1000 L . Furthermore, we find evidence from far-infrared molecular spectra and 3.6 cm emission that FIR 4 drives an outflow. The final stellar mass the protostar will ultimately achieve is uncertain due to its association with the large reservoir of mass found in the cold core.

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“…Images at 350 and 870 μm were acquired at APEX with SABOCA and LABOCA, respectively. The observing and data reduction procedures for the APEX images are described in Stanke et al (2010). Figure 1 shows a composite of the final map created using Method 2 for the 70 and 160 μm PACS channels.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Herschel-PACS imaging of protostars in the HH 1–2 outflow complex

Fischer¹,

Megeath²,

Ali

et al. 2010

A&A

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We present 70 and 160 μm Herschel science demonstration images of a field in the Orion A molecular cloud that contains the prototypical Herbig-Haro objects HH 1 and 2, obtained with the Photodetector Array Camera and Spectrometer (PACS). These observations demonstrate Herschel's unprecedented ability to study the rich population of protostars in the Orion molecular clouds at the wavelengths where they emit most of their luminosity. The four protostars previously identified by Spitzer 3.6-40 μm imaging and spectroscopy are detected in the 70 μm band, and three are clearly detected at 160 μm. We measure photometry of the protostars in the PACS bands and assemble their spectral energy distributions (SEDs) from 1 to 870 μm with these data, Spitzer spectra and photometry, 2MASS data, and APEX sub-mm data. The SEDs are fit to models generated with radiative transfer codes. From these fits we can constrain the fundamental properties of the protostars. We find luminosities in the range 12-84 L and envelope densities spanning over two orders of magnitude. This implies that the four protostars have a wide range of envelope infall rates and evolutionary states: two have dense, infalling envelopes, while the other two have only residual envelopes. We also show the highly irregular and filamentary structure of the cold dust and gas surrounding the protostars as traced at 160 μm.

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Hier ist wahrhaftig ein Loch im Himmel

Cited by 26 publications

References 21 publications

The Evolution of Far-Infrared Co Emission From Protostars

The Evolution of Far-Infrared Co Emission From Protostars

On the Nature of the Deeply Embedded Protostar Omc-2 Fir 4

Herschel-PACS imaging of protostars in the HH 1–2 outflow complex

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