The AzTEC mm-wavelength camera

Wilson, G. W.; Austermann, J. E.; Perera, Thushara; Scott, K. S.; Ade, Peter A. R.; Bock, J. J.; Glenn, J.; Golwala, S. R.; Kim, S.; Kang, Yun Hee; Lydon, Donald S.; Mauskopf, Philip Daniel; Predmore, C. R.; Roberts, C.; Souccar, Kamal; Yun, Min S.

doi:10.1111/j.1365-2966.2008.12980.x

Cited by 160 publications

(133 citation statements)

References 15 publications

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“…The principal component analysis (PCA) (Scott et al 2008) cleaning method was applied to remove atmospheric noise. Details of the flux calibration are described by Wilson et al (2008) and Scott et al (2008). Since the PCA method does not preserve the extended components reliably, we applied the iterative mapping method FRUIT (Liu et al 2010;Shimajiri et al 2011) to recover the extended components.…”

Section: Aztec/astementioning

confidence: 99%

“…From 2008 October to November, we carried out 1.1 mm dustcontinuum observations towards L1642 with the AzTEC camera (Wilson et al 2008) on the ASTE 10 m telescope (Ezawa et al 2004;Kohno et al 2004) located at Pampa la Bola, Chile, at an altitude of 4800 m. The AzTEC camera temporarily mounted on the ASTE telescope is a 144-element bolometric camera tuned to operate in the 1.1 mm atmospheric window, which provides a FWHM resolution of 28 (Wilson et al 2008). Observations were performed in raster-scan mode.…”

Section: Aztec/astementioning

confidence: 99%

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Multiwavelength study of the high-latitude cloud L1642: chain of star formation

Malinen

Juvela

Zahorecz

et al. 2014

A&A

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Context. L1642 is one of the two high galactic latitude (|b| > 30 • ) clouds confirmed to have active star formation. Aims. We examine the properties of this cloud, especially the large-scale structure, dust properties, and compact sources at different stages of star formation.Methods. We present high-resolution far-infrared and submillimetre observations with the Herschel and AKARI satellites and millimetre observations with the AzTEC/ASTE telescope, which we combined with archive data from near-and mid-infrared (2MASS, WISE) to millimetre wavelength observations (Planck).Results. The Herschel observations, combined with other data, show a sequence of objects from a cold clump to young stellar objects (YSOs) at different evolutionary stages. Source B-3 (2MASS J04351455-1414468) appears to be a YSO forming inside the L1642 cloud, instead of a foreground brown dwarf, as previously classified. Herschel data reveal striation in the diffuse dust emission around the cloud L1642. The western region shows striation towards the NE and has a steeper column density gradient on its southern side. The densest central region has a bow-shock like structure showing compression from the west and has a filamentary tail extending towards the east. The differences suggest that these may be spatially distinct structures, aligned only in projection. We derive values of the dust emission cross-section per H nucleon of σ e (250 μm) = 0.5−1.5 × 10 −25 cm 2 /H for different regions of the cloud. Modified black-body fits to the spectral energy distribution of Herschel and Planck data give emissivity spectral index β values 1.8-2.0 for the different regions. The compact sources have lower β values and show an anticorrelation between T and β. Conclusions. Markov chain Monte Carlo calculations demonstrate the strong anticorrelation between β and T errors and the importance of millimetre wavelength Planck data in constraining the estimates. L1642 reveals a more complex structure and sequence of star formation than previously known.

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Section: Aztec/astementioning

confidence: 99%

Section: Aztec/astementioning

confidence: 99%

Multiwavelength study of the high-latitude cloud L1642: chain of star formation

Malinen

Juvela

Zahorecz

et al. 2014

A&A

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“…We carried out 1.1 mm dust-continuum observations toward the B59 region with the AzTEC camera (Wilson et al 2008) mounted on the ASTE 10 m telescope (Ezawa et al 2004;Kohno et al 2004) located at Pampa la Bola (altitude = 4800 m), Chile. The observations were performed over the period 2008 October 17-31.…”

Section: Aztec/aste Observationsmentioning

confidence: 99%

The Rotating Outflow, Envelope, and Disk of the Class-0/I Protostar [Bhb2007]#11 in the Pipe Nebula

Hara

Shimajiri

Tsukagoshi

et al. 2013

ApJ

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We present the results of observations toward a low-mass Class-0/I protostar [BHB2007]#11 (B59#11) in the nearby (d = 130 pc) star-forming region Barnard 59 (B59), in the Pipe Nebula. We utilize the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope (∼22 resolution), focusing on the CO(3-2), HCO + , H 13 CO + (4-3), and 1.1 mm dust-continuum emission transitions. We also show Submillimeter Array (SMA) data with ∼5 resolution in 12 CO, 13 CO, C 18 O(2-1), and 1.3 mm dust-continuum emission. From ASTE CO(3-2) observations, we found that B59#11 is blowing a collimated outflow whose axis lies almost on the plane of the sky. The outflow traces well a cavity-like structure seen in the 1.1 mm dust-continuum emission. The results of SMA 13 CO and C 18 O(2-1) observations have revealed that a compact and elongated structure of dense gas is associated with B59#11; the structure is oriented perpendicular to the outflow axis. There is a compact dust condensation with a size of 350 × 180 AU seen in the SMA 1.3 mm continuum map, and the direction of its major axis is almost the same as that of the dense gas elongation. The distributions of 13 CO and C 18 O emission also show velocity gradients along their major axes, which are thought to arise from the envelope/disk rotation. From detailed analysis of the SMA data, we infer that B59#11 is surrounded by a Keplerian disk with a radius of less than 350 AU. In addition, the SMA CO(2-1) image shows a velocity gradient in the outflow in the same direction as that of the dense gas rotation. We suggest that this velocity gradient indicates rotation in the outflow.

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“…-the Sub-millimeter Common User Bolometer Array (SCUBA, Holland et al 1999) "supermap" of 35 SMGs selected to have data of S /N ≥ 4 at 850 μm (Borys et al 2003;Pope et al 2005Pope et al , 2006; -the Max Planck Millimeter Bolometer Array (MAMBO, IRAM 30-m telescope, Bertoldi et al 2000) 1200 μm map from Greve et al (2008), composed by 27 sources detected with 3.5 ≤ S /N < 4 and 20 with S /N ≥ 4; -the AzTEC (Wilson et al 2008, 15 m James Clerk Maxwell Telescope -JCMT) 1100 μm map of 28 sources detected with S /N ≤ 3.75 ).…”

Section: Sub-mm Detections: a Large Population Of Massive Starburst Gmentioning

confidence: 99%

Searching for massive galaxies at z ≥ 3.5 in GOODS-North

Mancini

Matute

Cimatti

et al. 2009

A&A

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Aims. We constrain the space density and properties of massive galaxy candidates at redshifts of z ≥ 3.5 in the Great Observatories Origin Deep Survey North (GOODS-N) field. By selecting sources in the Spitzer + IRAC bands, a sample highly complete in stellarmass is assembled, including massive galaxies that are very faint in the optical/near-IR bands and would be missed by samples selected at shorter wavelengths. Methods. The z ≥ 3.5 sample was selected to m AB = 23 mag at 4.5 μm using photometric redshifts obtained by fitting the galaxies spectral energy distribution at optical, near-IR bands, and IRAC bands. We also require that the brightest band (in AB scale) in which candidates are detected is the IRAC 8.0 μm band to ensure that the near-IR 1.6 μm (rest-frame) peak is falling in or beyond this band. Results. We found 53 z ≥ 3.5 candidates, of masses in the range M ∼ 10 10 −10 11 M . At least ∼81% of these galaxies are missed by traditional Lyman Break selection methods based on ultraviolet light. Spitzer + MIPS emission is detected for 60% of the sample of z ≥ 3.5 galaxy candidates. Although in some cases this might suggest a residual contamination from lower redshift starforming galaxies or Active Galactic Nuclei, 37% of these objects are also detected in the sub-mm/mm bands in SCUBA, AzTEC, and MAMBO surveys, and have properties fully consistent with vigorous starburst galaxies at z ≥ 3.5. The comoving number density of galaxies with stellar masses of above 5 × 10 10 M (a reasonable stellar-mass completeness limit for our sample) is 2.6 × 10 −5 Mpc −3 (using the volume within 3.5 < z < 5), and the corresponding stellar mass density is ∼(2.9 ± 1.5) × 10 6 M Mpc −3 , or about 3% of the local density above the same stellar mass limit. For the subsample of MIPS-undetected galaxies, we measure a number density of ∼0.97 × 10 −5 Mpc −3 and a stellar mass density of ∼(1.15 ± 0.7) × 10 6 M Mpc −3 . Even in the unlikely case that these are all truly quiescent galaxies, this would imply an increase in the space density of passive galaxies by a factor of ∼15 between z ∼ 4 and z = 2, and by ∼100 to z = 0.

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The AzTEC mm-wavelength camera

Cited by 160 publications

References 15 publications

Multiwavelength study of the high-latitude cloud L1642: chain of star formation

Multiwavelength study of the high-latitude cloud L1642: chain of star formation

The Rotating Outflow, Envelope, and Disk of the Class-0/I Protostar [Bhb2007]#11 in the Pipe Nebula

Searching for massive galaxies at z ≥ 3.5 in GOODS-North

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