5/21/2012 1 1 Instruments in Science and Education at Bosscha Observatory ITB, INDONESIA H. L. Malasan Bosscha Observatory, Faculty of Mathematics & Natural Sciences Institut Teknologi Bandung, Bandung, INDONESIA 5/21/2012 2 Major institutions constituting professional astronomers in Indonesia Institut Teknologi Bandung (ITB) National Institute of Aeronautics & Space (LAPAN) Meteorology, Climatology & Geophysical Agency (BMKG) 5/21/2012 3 5/21/2012 http://bosscha.itb.ac.id 5/21/2012 4
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Instruments in Science and
Education at Bosscha
Observatory ITB,
INDONESIA H. L. Malasan
Bosscha Observatory,
Faculty of Mathematics & Natural Sciences
Institut Teknologi Bandung,
Bandung, INDONESIA
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Major institutions constituting
professional astronomers in Indonesia
Institut Teknologi
Bandung
(ITB)
National Institute
of Aeronautics &
Space
(LAPAN)
Meteorology,
Climatology &
Geophysical
Agency
(BMKG)
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http://bosscha.itb.ac.id
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Bosscha Observatory in
Lembang
1073658 E 64932.93S, 1310 m above sea level
Lembang: 15 km north of Bandung, Mt. Tangkuban Perahu (2000 m, slightly active volcano) 8 km to the north
Typical seeing size=1−2, Vsky=18m/[]2
(Nugroho et al, 2006)
20 30 40 50
17.0
17.5
18.0
18.5
Sky Brightness Dependence with Altitude
Altitude
Sky
Mag
nitu
de in
V
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T e l e s c o p e s a t B o s s c h a O b s e r v a t o r y
Fakta & Data
Telescopes at Bosscha
Observatory up to 1989
Double 60cm Zeiss
refractor
71/51cm Schmidt
telescope)
37cm Bamberg
refractor
45cm GOTO Cassegrainian
reflector 5/21/2012 6
7
2000-
Reposition of Bosscha Observatory
as “the only” observatory in
Indonesia
Center for multidisciplinary area of
research in basic space science
Enhancement of outreach activities
to answer pressing demand on public
service
“Science” oriented “Science” and
“Value” oriented institution
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ASTRO
NOMY
Primary
Education
Secondary
Education Science
public
outreach
Research
Tertiary
Education
8 8
Small telescopes v.s.
Large telescope?
Networking observatories with “small”
telescopes
Astroeconomics model toward higher
productivity of (optical) data
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Astroeconomic model of network (Budding 1993) Cost-productivity for
group of telescopes
(characterized by D)
in remote/automated
fashion
1. Information flow
2. Key cost & organization
Advantages of small telescope: Efficiency
Adequacy Availability Flexibility
Serendipity
low capital
High capital
Relative knowledge rate WET
AAVSO
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Role of general-purpose small telescopes
(small telescope owner’s view)
Projects which require large number of observations
Projects which require all-sky or extended time coverage
Projects which require extreme flexibility
Stimulation for larger access ability to larger telescope
Training, experiment & development of (new) instrument
Education & outreach
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Extending capability of small-
intermediate size telescopes for
networking
Support of pointing & tracking for proper CCD imagery & spectroscopy
Autoguider
New control system based on common S/W Remote
Embedded acquistion system
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New GOTO Telescope
Controller Versi 1.0 (2005)
GOTO Telescope Controller
Versi 2.0 (2006)
Telescope Pointing
Analysis with new
control software
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13
Proliferation of small telescopes at the
Observatory and new public facility
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Bosscha Observatory: Evolution of astronomical data acquisition system
Sp
PMT
CCD
1989
2000
1982 1989
1994
1999-2003
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The Bosscha-Gunma
Compact Spectrographs
Type : Slit and plane grating
Configuration : Quasi-Littrow (=30)
Slit width : 80 m
Slit length : >20 mm
Slit position : Fixed
Collimator and
Camera
: Lens system
Collimator optics : f=240 mm
Camera optics : f=200 mm
Collimated beam
size
: 20mm (at f/12), 13.3 mm (at
f/18)
Gratings : 300 grooves/mm blazed at
500 nm
1200 grooves/mm blazed
at 500 nm
Order-cut filters : Short-cut at 390 nm and 480
nm
Comparison
source
: Fe-Ar-Ne
Basic pupils : Slit viewer
Main eyepiece
Dimension : 30 cm (l) 20 cm (w) 27
cm (h)
Weight : 15 kgf. (without camera)
Overal
throughput
: 10%
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Creation of homogeneous data
handling and analysis system
Hardwares:
Sun Ultra (Unix)
PCs running Linux
Large storage system
(GBytes)
IRAF (+IDL+GDL)
Data sharing and
handling at the same
level
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Bosscha Computer Cluster - Microwulf
Head Node
Node 1
Node 2
Node 3
internet
switch
Head Node Proc : 3.2 GHz
Memory : 1GB PC 5300
HDD: 1 TB + 80GB
Optical Drive : DVD-ROM
Node 1 Proc : 2.4 GHz
Memory : 512MB
Node 2 Proc : 2.4 GHz
Memory : 512MB
Node 3 Proc : 2.4 GHz
Memory : 2x256MB
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GAO-ITB Remote Telescope System (2005)
D=8 inches
f/D=10.0
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Astronomers & Students at the Observatory
carry out researches in various fields
Optical (Double star) Astrometry
Optical Photometry and Spectroscopy:
Stars, Solar system, interstellar mater
Radio Astronomy: Galaxy, Sun
Computer Network and Computer Cluster
Education and Popularization
Development of scientific instruments
Development of acquisition systems
Main activities of the Observatory :
1. investigation of orbits, determination of
masses of double stars.
2. Photometry and spectroscopy
3. Solar observation
4. Target opportunity objects
Common methods :
• Observation and gathering of
astronomical data
• Reduction of the obtained data
• Analysis of the reduced data
• Writing and Publish paper
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N
E
1
N
E
1
N
E
1
Asteroid (249) Ilse was observed on
2006 August 31 at the Bosscha
Observatory using SBIG CCD ST8-XME
attached to the Goto 45-cm telescope.
The upper, middle, and lower panels
were taken, respectively, on 15:32,
15:38, and 15:44 UT. The asteroid is
denoted by an arrow in each panel.
Observers: B. Dermawan, S. Siregar
Exp. Time: 120 s, Filter: R
Rmag = 13.2
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BVRI photometry of a 10-th mag eclipsing
binary BW Eri with GAO-ITB RTS + 20.3
cm telescopes, low resolution spectroscopy
with 45-cm GOTO telescope (Kristyowati et
al 2006)
B
V
R
I
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CCD Photometry of 7th mag RS Gru with GAO-ITB
RTS, spectroscopy with GOTO (Prasetyono, 2006)
Phase=0.0 Phase=0.5
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CCD observation of extrasolar planet transit using
GAO-ITB RTS and GOTO (Satyaningsih et al.
2006)
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The observed transit phenomenon
produces a dimming of the star HD
209458 of less than 2%
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CCD photometry of open cluster Ro6 with 28-cm
Schmidt Cassegrain telescope (Kuncarayakti et al.
2006)
V-band image of Ro 6
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Nova V1280 Sco (Kuncarayakti et al. 2007)
observed using 10’ telescope
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Productive
small
telescope for
emission line
spectroscopy
(Bosscha
Obs-Koyama
Astroph Obs,
Aug 2011)
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Electronic Telegram No. 2796
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
CBAT Director: Daniel W. E. Green; Hoffman Lab 209; Harvard University;
Prepared using the Tamkin Foundation Computer Network
PR LUPI = NOVA LUPI 2011 = PNV J14542000-5505030
Nicholas J. Brown, Two Rocks, Western Australia, reports his discovery of a possible nova (mag 10.2) on two TMax 400 films taken on Aug. 4.73 UT using a 135-mm-f.l. f/2
Canon camera lens. Brown's approximate position for the variable is R.A. = 14h54m20s, Decl. = -55d05'03" (equinox 2000.0); he notes that nothing brighter than mag 11.7
appears on a film that he took on July 5.85. The variable was designated PNV J14542000-5505030 when it was posted on the Central Bureau's TOCP webpage, and based on
the spectroscopic reports confirming the object as a nova (see below), it has been assigned the permanent GCVS designation PR Lup by N. N. Samus. Ernesto Guido, Nick
Howes, and Giovanni Sostero report that a CCD image taken of PR Lup remotely through the 2.0-m f/10 Ritchey-Chretien "Faulkes Telescope South" (+ Bessel R filter) on Aug.
13.5 shows it at mag 8.4 and at position R.A. = 14h54m23s.09, Decl. = -55d05'11".2 (equinox 2000.0; USNO-B1.0 catalogue reference stars). Guido et al. have posted a color
image at website URL http://bit.ly/onysAh, and a comparison of their image with a Digitized Sky Survey R plate from 1999 is posted at http://bit.ly/pUq8jd.
Additional magnitudes for PR Lup (visual unless otherwise noted): July 20.042 UT, [11.5 (W. Liller, Vina del Mar, Chile; 85-mm-f.l. Nikon lens + Tech Pan film + orange filter);
July 25.989, 11.1 (Liller); Aug. 1.008, 10.4 (Liller); Aug. 8.040, 10.3 (A. Amorim, Florianopolis, Brazil; moonlight); Aug. 8.066, 10.3 (Gonzalo Vargas Beltran, Cochabamba,
Bolivia; via E. Waagen, AAVSO); Aug. 8.375, 10.3 (R. Stubbings, Tetoora Road, Victoria, Australia; via Waagen); Aug. 12.443, 9.6 (Joseph Brimacombe, Cairns, Australia;
remotely using a 40-cm RCOS telescope + U9000 CCD camera at Macedon Ranges Observatory,Melbourne, Australia; position end figures 23s.06, 11".2; image posted at
website URL http://www.flickr.com/photos /43846774@N02/6041126507/); Aug. 13.988, 8.5 (Liller).
F. M. Walter, Stony Brook University, reports that Brown's suspected nova is indeed an "Fe II"-type nova. Photometric and spectroscopic observations were obtained using
the SMARTS/Cerro Tololo facilities, starting on Aug. 9 UT. Photometry with the 1.3-m telescope (+ ANDICAM dual-channel photometer) shows maximum light (V = 9.1, K = 6.2)
on Aug. 13.02 (+1/-2 days). By Aug. 23.0, the nova had faded to V = 11.2 and K = 8.1. Optical spectroscopy with the 1.5-m telescope (+ RC specrograph) at a variety of
resolutions between Aug. 9.0 and 22.0 shows the spectrum of a classical "Fe II"-type nova near maximum light. Near photometric maximum, on Aug. 12.0, the blue spectrum
(range 365-540 nm; 0.43-nm resolution) showed strong emission, with P-Cyg absorption, in the Balmer series H-beta through H_11, Ca II K, and the Fe II multiplets 42 and
49. At this resolution, a single absorption component is seen, at a velocity of about -1100 km/s. On Aug. 13.98, H-alpha had an emission equivalent-width of -17.0 nm, with P-
Cyg absorption at -1100 km/s. Low-dispersion (1.7-nm resolution) spectra covering the full optical range on Aug. 16.97 and 22.04 show strong emission from O I
630.0-, 777.4-, and 844.6-nm; C II 732.5-nm; and the Ca infrared triplet. As of Aug. 22.0, no helium lines were obvious, and no high-temperature lines had appeared.
H. L. Malasan, J. Suherli, and E. Wiyando, Bosscha Observatory, Institut Teknologi Bandung, Indonesia; and A. Arai and H. Kawakita, Koyama Astronomical Observatory,
Kyoto Sangyo University, Japan, report on optical spectroscopic observations (R about 400) of PNV J14542000-5505030 = PR Lup on Aug. 16.6 UT at Bosscha Observatory
using a 20-cm Schmidt-Cassegrain telescope (+ SBIG DSS7 spectrograph). The spectra exhibit strong H-alpha, H-beta, and Fe II multiplet emissions, suggesting that the
variable is a "Fe II"-type classical nova. P-Cygni profiles are absent, and the FWHM of the H-alpha emission is about 1700 km/s.
NOTE: These 'Central Bureau Electronic Telegrams' are sometimes
superseded by text appearing later in the printed IAU Circulars.