The Herschel Orion Protostar Survey: Luminosity and Envelope Evolution

Fischer, William J.; Megeath, S. Thomas; Furlan, Elise; Ali, B.; Stutz, Amelia M.; Tobin, John J.; Osorio, M. R. Zapatero; Stanke, T.; Manoj, P.; Poteet, C. A.; Booker, Joseph; Hartmann, L.; Wilson, Thomas L.; Myers, Philip C.; Watson, D. M.

doi:10.3847/1538-4357/aa6d69

Cited by 88 publications

(101 citation statements)

References 68 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We compiled an initial sample of young stellar objects (YSOs) on the basis that they were classified as Class II objects in Megeath et al (2012Megeath et al ( , 2016 and were located in L1641 (we require that our sample be located below -6 • declination, see Figure 1). For this sample, we extracted photometry from the Herschel Orion Protostar Survey (HOPS) open-time key program in 2010 and 2011 (e.g., Manoj et al 2013;Stutz et al 2013;Furlan et al 2016;Fischer et al 2017;B. Ali et al 2018, submitted).…”

Section: Observationsmentioning

confidence: 99%

“…We present Herschel Space Observatory 8 (Pilbratt et al 2010) photometry taken with the Photodetector Array Camera and Spectrometer (PACS; Poglitsch et al 2010) of 104 Class II objects in L1641. These protoplanetary disks were observed as part of the Herschel Orion Protostar Survey (HOPS), an open-time key program (e.g., Manoj et al 2013;Stutz et al 2013;Furlan et al 2016;Fischer et al 2017;B. Ali et al 2018, submitted).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Herschel Observations of Protoplanetary Disks in Lynds 1641*

Grant

Espaillat

Megeath

et al. 2018

ApJ

Self Cite

View full text Add to dashboard Cite

We analyze Herschel Space Observatory observations of 104 young stellar objects with protoplanetary disks in the ∼1.5 Myr star-forming region Lynds 1641 (L1641) within the Orion A Molecular Cloud. We present spectral energy distributions from the optical to the far-infrared including new photometry from the Herschel Photodetector Array Camera and Spectrometer (PACS) at 70 µm. Our sample, taken as part of the Herschel Orion Protostar Survey, contains 24 transitional disks, eight of which we identify for the first time in this work. We analyze the full disks with irradiated accretion disk models to infer dust settling properties. Using forward modeling to reproduce the observed n K S −[70] index for the full disk sample, we find the observed disk indices are consistent with models that have depletion of dust in the upper layers of the disk relative to the midplane, indicating significant dust settling. We perform the same analysis on full disks in Taurus with Herschel data and find that Taurus is slightly more evolved, although both samples show signs of dust settling. These results add to the growing literature that significant dust evolution can occur in disks by ∼1.5 Myr.

show abstract

Section: Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Herschel Observations of Protoplanetary Disks in Lynds 1641*

Grant

Espaillat

Megeath

et al. 2018

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…However, Kenyon et al (1990) found that luminosities of most protostars fall far below those expected from energy release by steady accretion over protostellar lifetimes. This luminosity problem has since been confirmed with an improved census of protostars (e.g., Enoch et al 2009;Dunham et al 2010; see also discussions in Dunham et al 2014 andFischer et al 2017).…”

Section: Introductionmentioning

confidence: 83%

“…The resolution of the luminosity problem likely requires either a time-dependent or mass-dependent accretion rate (e.g., discussions in Hartmann et al 2016 andFischer et al 2017; see also, e.g., Offner & McKee 2011;Myers 2012). Observationally, strong but mostly indirect evidence suggests that the accretion rate is punctuated by short bursts of rapid accretion, often termed episodic accretion (Kenyon et al 1990;Dunham et al 2010;Dunham & Vorobyov 2012).…”

Section: Introductionmentioning

confidence: 99%

How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions

Herczeg

Johnstone

Mairs

et al. 2017

ApJ

View full text Add to dashboard Cite

Most protostars have luminosities that are fainter than expected from steady accretion over the protostellar lifetime. The solution to this problem may lie in episodic mass accretion-prolonged periods of very low accretion punctuated by short bursts of rapid accretion. However, the timescale and amplitude for variability at the protostellar phase is almost entirely unconstrained. In A James Clerk Maxwell Telescope/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions, we are monitoring monthly with SCUBA-2 the submillimeter emission in eight fields within nearby ( 500 < pc) star-forming regions to measure the accretion variability of protostars. The total survey area of ∼1.6 deg 2 includes ∼105 peaks with peaks brighter than 0.5 Jy/ beam (43 associated with embedded protostars or disks) and 237 peaks of 0.125-0.5 Jy/beam (50 with embedded protostars or disks). Each field has enough bright peaks for flux calibration relative to other peaks in the same field, 1 which improves upon the nominal flux calibration uncertainties of submillimeter observations to reach a precision of ∼2%-3% rms, and also provides quantified confidence in any measured variability. The timescales and amplitudes of any submillimeter variation will then be converted into variations in accretion rate and subsequently used to infer the physical causes of the variability. This survey is the first dedicated survey for submillimeter variability and complements other transient surveys at optical and near-IR wavelengths, which are not sensitive to accretion variability of deeply embedded protostars.

show abstract

“…These sources may be similar in nature to the 70 µm protostars (Stutz et al (2013); see also Ragan et al 2012). These authors concluded that protostars with very red 70 µm to 24 µm colors are consistent with having denser envelopes and thus are younger than the bulk of the Class 0 and Class I protostars in Orion (Furlan et al 2016;Fischer et al 2017). To examine if these bright sources are YSO candidates, we conducted the fitting of spectral energy distribution (SED) with the tool developed by Robitaille et al (2006).…”

Section: Star Formation In the Filamentsmentioning

confidence: 88%

The straight and isolated G350.54+0.69 filament: density profile and star formation content

Liu

Stutz

Yuan

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We investigate the global properties of the straight and isolated filamentary cloud G350.54+0.69 using Herschel continuum and APEX molecular line data. The overall straight morphology is similar to two other well studied nearby filaments (Musca and Taurus-B211/3) while the isolated nature of G350.54+0.69 appears similar to Musca. G350.54+0.69 is composed of two distinct filaments with a length ∼ 5.9 pc for G350.5-N (∼ 2.3 pc for G350.5-S), a total mass of ∼ 810 M (∼ 110 M ), and a mean temperature of ∼ 18.2 K (∼ 17.7 K). We identify 9 dense and gravitationally bound cores in the whole cloud G350.54+0.69. The separations between cores and the line mass of the whole cloud appear to follow the predictions of the "sausage" instability theory, which suggests that G350.54+0.69 could have undergone radial collapse and fragmentation. The presence of young protostars is consistent with this hypothesis. The line masses of the two filaments (∼ 120 M pc −1 for G350.5-N, and ∼ 45 M pc −1 for G350.5-S), mass-size distributions of the dense cores, and low-mass protostars collectively suggest that G350.54+0.69 is a site of ongoing low-mass star formation. Based on the above evidence, we place G350.54+0.69 in an intermediate evolutionary state between Musca and Taurus-B211/3. We suggest that investigations into straight (and isolated) versus those distributed inside molecular clouds may provide important clues into filament formation and evolution.2 Hi-GAL, the Herschel infrared Galactic Plane Survey, is an Open Time Key project on the Herschel Space Observatory (HSO) aiming to map the entire Galactic Plane in five infrared bands. This survey covers a |b| < 1 • wide strip of the Milky Way Galactic plane in the longitude range −60 • < l < 60 • .

show abstract

The Herschel Orion Protostar Survey: Luminosity and Envelope Evolution

Cited by 88 publications

References 68 publications

Herschel Observations of Protoplanetary Disks in Lynds 1641*

Herschel Observations of Protoplanetary Disks in Lynds 1641*

How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions

The straight and isolated G350.54+0.69 filament: density profile and star formation content

Contact Info

Product

Resources

About