AzTEC 1.1 mm OBSERVATIONS OF THE MBM12 MOLECULAR CLOUD

Kim, M.J.; Kim, S.; Youn, S.; Yun, Min S.; Wilson, Grant; Aretxaga, I.; Williams, Jonathan P.; Hughes, D. H.; Humphrey, A.; Austermann, J. E.; Perera, Thushara; Mauskopf, Philip Daniel; Magnani, L.; Kang, Yun Hee

doi:10.1088/0004-637x/746/1/11

Cited by 5 publications

(2 citation statements)

References 43 publications

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“…This should produce a result identical to the analysis shown in a much simpler fashion. This paper documents the technique used in several AzTEC publications in 2011–2012 (Aretxaga et al 2011; Humphrey et al 2011; Yun et al 2011; Kim et al 2012). If the technique is revised further to include this suggestion or others, it will be documented in subsequent publications.…”

Section: Future Workmentioning

confidence: 97%

Calculating the transfer function of noise removal by principal component analysis and application to AzTEC deep-field observations

Downes¹,

Welch²,

Scott³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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Instruments using arrays of many bolometers have become increasingly common in the past decade. The maps produced by such instruments typically include the filtering effects of the instrument as well as those from subsequent steps performed in the reduction of the data. Therefore interpretation of the maps is dependent upon accurately calculating the transfer function of the chosen reduction technique on the signal of interest. Many of these instruments use non-linear and iterative techniques to reduce their data because such methods can offer an improved signal-to-noise ratio over those that are purely linear, particularly for signals at scales comparable to that subtended by the array. We discuss a general approach for measuring the transfer function of principal component analysis on point sources that are small compared to the spatial extent seen by any single bolometer within the array. The results are applied to previously released AzTEC catalogues of the Cosmic Evolution Survey (COSMOS), Lockman Hole, Subaru XMM-Newton Deep Field, Great Observatories Origins Deep Survey (GOODS)-North and GOODS-South fields. Source flux density and noise estimates increase by roughly +10 per cent for fields observed while AzTEC was installed at the Atacama Submillimeter Telescope Experiment and +15-25 per cent while AzTEC was installed at the James Clerk Maxwell Telescope. Detection significance is, on average, unaffected by the revised technique. The revised photometry technique will be used in subsequent AzTEC releases.

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Section: Future Workmentioning

confidence: 97%

Calculating the transfer function of noise removal by principal component analysis and application to AzTEC deep-field observations

Downes¹,

Welch²,

Scott³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…The activity of P/2012 F5 (Stevenson et al 2012;Moreno et al 2012), 596 (Hsieh et al 2012a;Ishiguro et al 2011a,b;Jewitt et al 2011;Moreno et al 2012), and P/2010 A2 (Jewitt et al 2010;Snodgrass et al 2010;Jewitt et al 2011;Hainaut et al 2012b;Kim et al 2012;Kleyna et al 2013) has been interpreted as the effect of impacts by small asteroids.…”

Section: Introductionmentioning

confidence: 99%

Continued activity in P/2013 P5 PANSTARRS

Hainaut

Boehnhardt

Snodgrass

et al. 2014

A&A

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The object P/2013 P5 PANSTARRS was discovered in August 2013, displaying a cometary tail, but its orbital elements indicated that it was a typical member of the inner asteroid main belt. We monitored the object from 2013 August 30 until 2013 October 05 using the CFHT 3.6 m telescope (Mauna Kea, HI), the NTT (ESO, La Silla), the CA 1.23 m telescope (Calar Alto), the Perkins 1.8m (Lowell) and the 0.6 m TRAPPIST telescope (La Silla). We measured its nuclear radius to be r < ∼ 0.25−0.29 km, and its colours g − r = 0.58 ± 0.05 and r − i = 0.23 ± 0.06, typical for an S-class asteroid, as expected for an object in the inner asteroid belt and in the vicinity of the Flora collisional family. We failed to detect any rotational light curve with an amplitude <0.05 mag and a double-peaked rotation period <20 h. The evolution of the tail during the observations was as expected from a dust tail. A detailed Finson-Probstein analysis of deep images acquired with the NTT in early September and with the CFHT in late September indicated that the object was active since at least late January 2013 until the time of the latest observations in 2013 September, with at least two peaks of activity around 2013 June 14 ± 10 d and 2013 July 22 ± 3 d. The changes of activity level and the activity peaks were extremely sharp and short, shorter than the temporal resolution of our observations (∼1 d). The dust distribution was similar during these two events, with dust grains covering at least the 1-1000 µm range. The total mass ejected in grains <1 mm was estimated to be 3.0 × 10 6 kg and 2.6 × 10 7 kg around the two activity peaks. Rotational disruption cannot be ruled out as the cause of the dust ejection. We also propose that the components of a contact binary might gently rub and produce the observed emission. Volatile sublimation might also explain what appears as cometary activity over a period of 8 months. However, while main belt comets best explained by ice sublimation are found in the outskirts of the main belt, where water ice is believed to be able to survive buried in moderately large objects for the age of the solar system deeply, the presence of volatiles in an object smaller than 300 m in radius would be very surprising in the inner asteroid belt.

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Large Particles in Active Asteroid P/2010 A2

Jewitt

Ishiguro

Agarwal

2013

ApJ

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Previously unknown asteroid P/2010 A2 rose to prominence in 2010 by forming a transient, comet-like tail consisting of ejected dust. The observed dust production was interpreted as either the result of a hypervelocity impact with a smaller body or of a rotational disruption. We have re-observed this object, finding that large particles remain a full orbital period after the initial outburst. In the intervening years, particles smaller than ∼3 mm in radius have been dispersed by radiation pressure, leaving only larger particles in the trail. Since the total mass is dominated by the largest particles, the radiation pressure filtering allows us to obtain a more reliable estimate of the debris mass than was previously possible. We find that the mass contained in the debris is ∼5×10 8 kg (assumed density 3000 kg m −3 ), the ratio of the total debris mass to the nucleus mass is ∼0.1 and that events like P/2010 A2 contribute <3% to the Zodiacal dust production rate. Physical properties of the nucleus and debris are also determined.

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AzTEC 1.1 mm OBSERVATIONS OF THE MBM12 MOLECULAR CLOUD

Cited by 5 publications

References 43 publications

Calculating the transfer function of noise removal by principal component analysis and application to AzTEC deep-field observations

Calculating the transfer function of noise removal by principal component analysis and application to AzTEC deep-field observations

Continued activity in P/2013 P5 PANSTARRS

Large Particles in Active Asteroid P/2010 A2

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