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PHEMU 2015 - PARIS 17-18 SEPTEMBER 2015 1
PHEMU 2015 - The Bucharest observational campaignRomanian Astronomical Institute of The Romanian Academy - AIRA
ADRIAN SONKA, MARCEL POPESCU, DAN ALIN NEDELCU, MIREL BIRLAN
PHEMU 2015 - PARIS 17-18 SEPTEMBER 2015 2
The Romanian Astronomical Institute of Romanian Academy
Main building Building of 0.5 meter telescope
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T05m telescope
Zeiss Cassegrain installed in 1964
Primary mirror • D = 0,5 m • F = 7,5 mm • F/D = 15
German Equatorial Mount
T05m at work
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CCD Camera
SBIG STL11000M
Size of chip: 36.1 x 24.7 mm
Size of chip: 4008 x 2745 pixels
Pixel size: 9 x 9 µm
UBVRI filter system
For PHEMU: unfiltered images
For PHEMU: binning 2x2
Resolution: 0.5 arcsec/pixel
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Typical PHEMU image
16.8 x 11.2 arcmin field
0.502 arcsec/pixel @Binning 2x2
Integration time: between 0.1 and 1 second
Jupiter usually is saturated
JupiterII IVI+II
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PHEMU PhotometryFor photometry we use Maxim Dl 5
For eclipses:
- The measured object: the satellite in eclipse
- The Reference object: satellite that does not take part in the eclipse
For occultations:
- The measured object: the satellites in occultation
- The Reference object: satellite that does not take part in the eclipse
Photometry during an eclipse3ecl1 – 16.02.2015
Photometry during an occultation3occ1 – 16.02.2015
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Our sky
Our telescope is surrounded by trees. The observatory is in a park
But the park is only 2 km away from town center
Visual magnitude limit is 4
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Our seeing – FWHM plot may 2014 – apr 2015
• FWHM measured for 10052 images
• Air mass not accounted
Cassegrain 0.5 m, f/15, SBIG STL11000MA. Sonka, M. Popescu, A. Nedelcu
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PHEMU 2015
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PHEMU 2015 We have observed 10 mutual phenomena:
- 5 occultations
- 5 eclipses
◦ 4 phenomena involving satellites 3 and 1◦ 1 involving 3 and 2◦ 2 involving 1 and 2◦ 1 involving 4 and 1◦ 2 involving 4 and 2
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PHEMU 2015 light curves
Light curves of phenomena observed at Romanian Astronomical Institute of The Romanian Academy
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PHEMU 2015 light curves
Light curves of phenomena observed at Romanian Astronomical Institute of The Romanian Academy
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PHEMU UT Start UT End Exp. time [s]
Measured satellite
Reference Satellite
Altitude [°]
Delta mag calculated -
IMCCE
Delta mag observed – unfiltered
ToM observed [JD]
3occ1 2014-12-22T01:07:06.000 2014-12-22T02:44:50.000 0.5 3 and 1 2 60 0.46 0.46 2457013.5924
3ecl1 2015-02-02T18:15:44.414 2015-02-02T18:40:04.803 0.5 3 and 1 2 29 0.49 0.27 2457056.2646
3occ1 2015-02-02T18:15:44.414 2015-02-02T18:40:04.803 0.5 3 and 1 2 29 0.26 0.3 2457056.2742
3occ1 2015-02-16T23:03:23.000 2015-02-16T23:37:31.000 0.1 3 and 1 2 56 0.45 0.55 2457070.4734
3ecl1 2015-02-16T23:38:09.000 2015-02-17T00:03:09.000 0.1 1 2 52 0.57 2.23 2457070.4974
4occ2 2015-02-26T19:52:54.000 2015-02-26T20:41:47.000 0.1 4 and 2 3 62 0.17 0.22 2457080.3528
1occ2 2015-02-26T22:14:12.000 2015-02-26T22:27:06.000 0.1 1 and 2 3 58 0.10 0.1 2457080.4314
4ecl2 '2015-02-26T22:40:35.000 2015-02-26T22:59:40.000 0.1 2 3 55 0.95 0.8 2457080.4503
4ecl1 2015-02-26T23:37:25.000 2015-02-26T23:53:58.000 1 1 3 46 0.07 not detected -
1ecl2 2015-03-23T18:40:58.000 2015-03-23T18:53:07.000 0.1 2 3 65 0.63 1.4 2457105.2840
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Other interests• Minor planet photometry, spectroscopy
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Minor planet photometry
Between summer of 2014 and
autum of 2015 we have
observed 7 minor planets (4
NEA and 3 Main Belt)
For lightcurve study we use
MPO Canopus
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(137170) 1999 HF1• Observations between 21.05-14.06.2014• 6 nights of observations• A total of 22 hours of observations• Longest night of 4.4 hours of observations• Minor planet magnitude: 15.5• Minor planet phase: 64-79°• Exposure 60s, clear filter
Results:• Period: 2.3188 +/- 0,0006 hours• Amplitude: 0.22 mag• Published in Minor Planet Bulletin Vol. 41, No. 4, pp. 285-286 (2014)
1991 HF1 TRAIL ON JUNE, 9TH 2014
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LCDB (Rev. 2015-May); Warner et al., 2009
Rotation Period: 2.3192 h LCDB (Rev. 2015-May); Warner et al., 2009
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(1114) Lorraine• Observations between 29.07-20.10.2014• 18 nights of observations• A total of 64 hours of observations• Longest night of 4.6 hours of observations• Minor planet magnitude: 14.5• Minor planet phase: -10 - + 17°• Exposure 60s, clear filter
Results:• Not yet published LORRAINE TRAIL ON AUGUST, 29TH 2014
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Rotation Period: 33: h [Behrend, R. (2005) Observatoire de Geneve
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(2649) Oongaq• Observations between 24.09-19.10.2014• 11 nights of observations• A total of 72 hours of observations• Longest night of 7 hours of observations• Minor planet magnitude: 15.4• Minor planet phase: -14 - + 23°• Exposure 60s, clear filter
Results:• Period: 2.789 +/- 0.006 hours• Amplitude: 0.44 mag• Not yet published
OONGAQ TRAIL ON OCTOBER, 5TH 2014
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(656) Beagle• Observations between 10.02-24.03.2015• 9 nights of observations• A total of 46 hours of observations• Longest night of 5.6 hours of observations• Minor planet magnitude: 14• Minor planet phase: -8 - + 9°• Exposure 60s, V filter
Results:• Period: 7.034 +/- 0.003 hours• Amplitude: 0,22 mag• Not yet published
BEAGLE TRAIL ON FEBRUARY, 20TH 2015
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Efficient network science
The case of 2004 BL86 (PHA):- Grazed the Earth : Jan 26, 2015- Distance: 1.2 million km.- Discovered in 2004 (LINEAR program)- Estimated diameter: 500m
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Circumstances
Regular awarded observing time:
- Isaac Newton telescope (2.5m aperture), Canary (Visible spectroscopy)-IRTF (3m aperture), Hawaii (infrared
0.8-2.5 µm spectroscopy)
Remote observing from Paris & Bucharest Cluj-Napoca Observatory performed photometry & derived rotational period for this object
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Spectroscopy
Successful observing runs in Feb 6 & 7, 2015, first spectrum of this PHA
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Analysis
- BL86 is V-type asteroidMineralogical analysis: 2004 BL86 has a basaltic mineralogyThermal albedo of BL86 help in deriving a diameter of 290 ± 20 m.
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Results
Spectroscopic analysis diminish by 40% the diameter previously estimated
Long term orbital integrations using clones show that 2004 BL86 is highly chaotic
No keyhole for hitting the Earth in the next five centuries Next favorable observation of 2004 BL86 in 2050!
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Astronomy & Astrophysics, August, 2015