Possible Future Spectroscopic Star Formation Surveys James Di Francesco (National Research Council Herzberg)

Herschel observations of the Sadavoy (2012)

JCMT Heterodyne Mapping Hardware ACSIS : “Auto-Correlation Spectral Imaging “Auto-Correlation Spectral Imaging System” System” 32-DCM correlator 32-DCM correlator 0.25 GHz to 1 GHz band widths 0.25 GHz to 1 GHz band widths up to 8192 channels up to 8192 channels HARP : “Heterodyne Array Receiver “Heterodyne Array Receiver Programme (for RxB band)” Programme (for RxB band)” 4 x 4 receptor focal-plane array 4 x 4 receptor focal-plane array covers GHz covers GHz 2’ x 2’ sky coverage 2’ x 2’ sky coverage first 345 GHz mapping system first 345 GHz mapping system HARP ACSIS

JCMT Gould Belt Survey: HARP GBS PLAN (250 hrs): map five ~30’ x 10’ areas map five ~30’ x 10’ areas (filaments) in: (filaments) in: - Orion A+B (Buckle et al. - Orion A+B (Buckle et al. 2010, 2012) 2010, 2012) - Serpens (Graves et al. 2010) - Serpens (Graves et al. 2010) - Taurus (Davis et al. 2010) - Taurus (Davis et al. 2010) - Ophiuchus (White et al. - Ophiuchus (White et al. 2014, submitted) 2014, submitted) plus GT or PI data of: plus GT or PI data of: - Perseus (Curtis et al. 2008) - Perseus (Curtis et al. 2008) - Pipe Nebula (Chrysostomou - Pipe Nebula (Chrysostomou et al. 2014, in prep) et al. 2014, in prep) L1495 in Taurus 12 CO 3-2: 12 CO 3-2: 0.3 K rms, 1 km s -1 ch’s 0.3 K rms, 1 km s -1 ch’s 13 CO C 18 O 3-2: 13 CO C 18 O 3-2: 0.3 K rms, 0.1 km s -1 ch’s 0.3 K rms, 0.1 km s -1 ch’s

Serpens: Outflow+ Kinematics 12 CO 3-2 traces outflows and C 18 O 3-2 traces dense material 12 CO 3-2 traces outflows and C 18 O 3-2 traces dense material complex C 18 O velocity structure argues against simple rotation, complex C 18 O velocity structure argues against simple rotation, instead due to shear or two-cloud collision? instead due to shear or two-cloud collision? Graves et al. 2010; Duarte-Cabral et al CO 3-2 (contours) C 18 O 3-2 (contours) C 18 O 3-2 (colors) 850 μm (greyscale) 850 μm (heatscale)

Future Spectroscopic Surveys 1.Expanding present GBS spectroscopic coverage 2.Mapping CO in High-mass Star-forming Regions 3.Tracing Mass Accumulation of Filaments and Cores 4.Exploring the Dense Interiors of Cores

1. Expanding GBS Coverage Drabek-Maunder et al. (2014, in prep.) In GBS, HARP observations covered only a small fraction of In GBS, HARP observations covered only a small fraction of area on sky SCUBA-2 observations covered area on sky SCUBA-2 observations covered slight “bias” toward known filamentary regions, as slight “bias” toward known filamentary regions, as necessitated by cancelled POL-2 program necessitated by cancelled POL-2 program

1. Expanding GBS Coverage Goals: Goals: - 12 CO 3-2: - 12 CO 3-2: probe outflows over all GBS areas where SCUBA-2 has probe outflows over all GBS areas where SCUBA-2 has now detected emission now detected emission - 13 CO C 18 O 3-2: - 13 CO C 18 O 3-2: trace kinematics of wider variety of cloud structures + trace kinematics of wider variety of cloud structures + expand possible sample of future POL-2 observations expand possible sample of future POL-2 observations Targets: Targets: - expanded areal coverage of Taurus, Ophiuchus, Perseus, - expanded areal coverage of Taurus, Ophiuchus, Perseus, Serpens, Orion? Serpens, Orion? - new coverage of clouds as yet unobserved: Cepheus, - new coverage of clouds as yet unobserved: Cepheus, IC5146, Auriga, Aquila, Scorpius, R CrA, northern Lupus IC5146, Auriga, Aquila, Scorpius, R CrA, northern Lupus Duration: hr, grade 2 weather Duration: hr, grade 2 weather

2. CO Mapping of High-mass SFRs NGC 7538 CO 3-2 Fallscheer et al. (2013) Many high-mass star-forming regions outside JPS and GBS, Many high-mass star-forming regions outside JPS and GBS, targets of new SCUBA-2 surveys? targets of new SCUBA-2 surveys? How are the kinematics of these clouds related to the How are the kinematics of these clouds related to the conditions that form high-mass stars? conditions that form high-mass stars? km/s km/s km/s

2. CO Mapping of High-mass SFRs Goals: Goals: - 12 CO 3-2 only: - 12 CO 3-2 only: probe outflows + gas kinematics over high-mass star- probe outflows + gas kinematics over high-mass star- forming regions (SFRs) at < 3 kpc forming regions (SFRs) at < 3 kpc IMPORTANT: determine CO contribution to SCUBA-2 IMPORTANT: determine CO contribution to SCUBA-2 fluxes in SFRs, has been seen be ~80%! fluxes in SFRs, has been seen be ~80%! Targets: Targets: - HOBYS fields: NGC 2264, MonR2, W48, Rosette, etc. - HOBYS fields: NGC 2264, MonR2, W48, Rosette, etc. - check the archive! - check the archive! - coordination with JPS needed - coordination with JPS needed Duration: 100 hr, grade 3 weather (grade 4 possible?) Duration: 100 hr, grade 3 weather (grade 4 possible?)

3. Mass Accumulation of Filaments Hacar et al. (2013) Ward-Thompson et al. (1996!) Filaments appear to be Filaments appear to be closely related to core closely related to core formation formation How fast do they grow? How fast do they grow? Need measurements of Need measurements of accretion rates accretion rates infall traced by infall traced by asymmetrically asymmetrically blue profiles blue profiles HCO + 4-3H 13 CO NGC 1333 IRAS 2

3. Mass Accumulation of Filaments Goals: Goals: - HCO / HCN 4-3: - HCO / HCN 4-3: optically thick line maps probe dense gas infall motions; optically thick line maps probe dense gas infall motions; BONUS: difference in line widths can probe magnetic BONUS: difference in line widths can probe magnetic field strengths (cf. Li & Houde 2008) field strengths (cf. Li & Houde 2008) - H 13 CO / H 13 CN H 13 CO / H 13 CN 4-3 optically thin lines provide “reference” to asymmetric optically thin lines provide “reference” to asymmetric HCO + and HCN profiles + trace flows (C 18 O enough?) HCO + and HCN profiles + trace flows (C 18 O enough?) Targets: Targets: - prominent GBS filaments: OMC-2/3, L1495-B211, Serpens - prominent GBS filaments: OMC-2/3, L1495-B211, Serpens South, Pipe Nebula? South, Pipe Nebula? Duration: hr, depending on no. and size of regions Duration: hr, depending on no. and size of regions

4. Dense Core Interiors Dense cores are very cold, Dense cores are very cold, leading to severe depletion leading to severe depletion of C-bearing molecules of C-bearing molecules Tracing core interiors can Tracing core interiors can be therefore difficult be therefore difficult H 2 D + does not deplete H 2 D + does not deplete (in fact, it can be quite (in fact, it can be quite enhanced at low T) enhanced at low T) H 2 D located H 2 D located at 372 GHz, within HARP at 372 GHz, within HARP range range Line is difficult to observe Line is difficult to observe due to atmospheric H 2 O due to atmospheric H 2 O line: need grade 1 weather line: need grade 1 weather Oph A Friesen, Di Francesco et al. (2014, submitted)

4. Dense Core Interiors Goals: Goals: - H 2 D : - H 2 D : yields kinematics of core interiors, yet can be extended yields kinematics of core interiors, yet can be extended provides “finding chart” for high-resolution ALMA data provides “finding chart” for high-resolution ALMA data - N 2 H + 4-3: - N 2 H + 4-3: a high density tracer that is also at 372 GHz, so can be a high density tracer that is also at 372 GHz, so can be observed “for free” with H 2 D , if excited; observed “for free” with H 2 D , if excited; can be compared with extensive N 2 H data of cores can be compared with extensive N 2 H data of cores Targets: Targets: - 25 concentrated (dense) pre-stellar or protostellar cores, - 25 concentrated (dense) pre-stellar or protostellar cores, - no wide-field mapping; 2’ x 2’ jiggles only - no wide-field mapping; 2’ x 2’ jiggles only Duration: 500 hr, depending on number of cores Duration: 500 hr, depending on number of cores

Summary The new JCMT partnership has an amazing tool for probing the kinematics of gas related to star formation: HARP + ACSIS: Further 12 CO / 13 CO / C 18 O studies of protostellar outflows Further 12 CO / 13 CO / C 18 O studies of protostellar outflows and dynamics in nearby clouds and dynamics in nearby clouds New 12 CO studies of same in high-mass clouds New 12 CO studies of same in high-mass clouds HCO + / HCN / H 13 CO + / H 13 CN studies of mass accumulation HCO + / HCN / H 13 CO + / H 13 CN studies of mass accumulation in filaments in filaments H 2 D + / N 2 H + studies of dense core interiors H 2 D + / N 2 H + studies of dense core interiors Total time: ~1500 hours, grades 1-3