| DATE: | 8 - 12 July, 2013 |
| VENUE: | Lecture Theatre T4, 1/F, Meng Wah Complex, The University of Hong Kong (Campus Map) |
LOCAL TOUR: |
Trip to the Hong Kong Global Geopark of China Date: 10 July 2013 PICK-UP Venue and Time: The University of Hong Kong, leaving around 1:00 p.m. FEE: HKD400/person DISMISSAL Venue: The University of Hong Kong Content: Visiting the Hong Kong Global Geopark of China, including places like Tung Ping Chau, the Double Haven. Dinner will be included. |
Public Talk at the Space Museum:
The Sky as Seen by the Fermi Gamma-ray Space TelescopePurpose of the Workshop:
The Fermi Gamma-ray Space Telescope has detected over thousand gamma-ray point sources. Nature of large percentage of these sources is still unknown. Most importantly data of Fermi is publicly available. The main purposes of this workshop include (1) to discuss new findings by using the data of Fermi satellite, (2) to promote collaboration among participants, especially the high energy astrophysicists in Asia and (3) to train the postgraduate students and postdocs to use the Fermi software to discover new sources.(I) Scientific Program:
Download Program (Updated on 9 July 2013, with presentation files added from time to time)(II) List of Participants:
(III) Discussion Topics:
(IV) Mini-training Course for Analysing Fermi Data
Instructors : Paul Ray, Pablo Saz Parkinson, Roberto Mignani, Andrea Belfiore, David Hui, Albert Kong, Eric Wu, Gene Leung and Jason WuThe hands-on workshop will involve exploration and analysis of multi-wavelength data with a focus on Fermi LAT data. All participants should install all the required tools in their laptop computers before attending the workshop. Analysis will be performed in a Linux-based (including Mac) environment. Participants should select the precompiled binaries of the tools that match their machine type. Here we provide the links for downloading and installing the required tools.
Fermi-LAT Package:
Fermi Science Tools: http://fermi.gsfc.nasa.gov/ssc/data/analysis/software/
Fermi-GBM Tool:
RMFIT: Installation Guide (v4.3.2, updated on 2/7/2013)
Optical Package:
IRAF: http://iraf.noao.edu/
INTEGRAL Package:
INTEGRAL OSA: http://www.isdc.unige.ch/integral/analysis#Software
INTEGRAL Data Download NEW
Pulsar Timing Package:
Tempo2 (with Fermi Plug-in): http://fermi.gsfc.nasa.gov/ssc/data/analysis/user/Fermi_plug_doc.pdf
Requirements for Pulsar Blind Search Session:
pyfits: http://www.stsci.edu/institute/software_hardware/pyfits
numpy: http://www.numpy.org/
Auxiliary Tools:
Image viewer ds9: http://hea-www.harvard.edu/RD/ds9/
HEASOFT: http://heasarc.gsfc.nasa.gov/lheasoft/download.html
Notes for Fermi Analysis
Notes for likelihood analysis
(V) Registration for Mini-Projects
Download (Updated on 15 July 2013)Scientific Organizing Committee
Local Organizing Committee
Sponsorship
Related Sites:
Online Registration Form (Registration Deadline: 26 May 2013)
Registration Fee: HK$2,000 (automatically waived for students and local participants. For academican, it may be waived upon request)We will acknowledge your registration within 5 working days upon receiving your registration.
Fermi LAT 0.5-20 GeV images of a 5o x 5o region centered on Terzan 5. The white circle shows the 95% confidence error circle of the gamma-ray source determined by using the 0.5-20 GeV image and gtfindsrc. The white crosses are the optical center of Terzan 5. In addition to Terzan 5, strong Galactic plane emission is also seen. Both images are smoothed by a 0.3o Gaussian function. The inset figures are the associated TS maps of the 2o x 2o region. All bright Fermi sources as well as the diffuse Galactic and extragalactic background emission are included in the background model. The black crosses denote the optical center of Terzan 5. (Kong et al 2010).
The X-ray and Optical orbital light curves of 1FGL J2339.7-0531 (Kong et al. 2012), which was later identified as a millisecond pulsar binary by (Ray et al. 2013).
Test-statistic (TS) map in 1-20 GeV of a region of 2o x 2o centered at the nominal position of Kes 17 (magenta cross). The peak emission of the southwestern and the eastern features are marked with a green cross. Positions of various sources are also illustrated. The color scale bar is used to indicate the TS values. The circle in black represents the 1σ positional error circle determined by gtfindsrc. (Wu et al 2011)
Fermi LAT γ-ray weighted light curve of M28A. A weight was assigned to each photon with the probability that it comes from M28 by using the task gtsrcprob in Fermi Science Tool. Two periods of rotation with a resolution of 40 phase bins per period is shown for clarity. The error bars of the light curve represent 1σ Poisson uncertainties. The shaded regions define the on-pulse intervals for Peak 1 and Peak 2. (Wu et al. 2013, ApJL in press)
Fermi LAT phase-resolved γ-ray count maps for events >0.2 GeV within 5o of the timing position of M28A (illustrated by the yellow cross). Top is north and left is east. The scale bar below shows the color scale of counts/pixel divided by the relevant phase interval. Top panel: Peak 1 region (i.e. 0.0<φ<0.4). Middle panel: Peak 2 region (i.e. 0.55<φ<0.75). Bottom panel: Off-pulse region (i.e. 0.4<φ<0.55 & 0.75<φ<1). The point source locates in the northeast of these maps is 2FGL J1833.6-2104 and the bright extended emission in the northwest is due to the diffuse γ-ray emission from the Galactic plane. (Wu et al. 2013)
(Left) Test-statistic (TS) map in 1-20 GeV of a region of 2o x 2o centered at the nominal position of HESS J1745-303. The color scale used to indicate the TS value is shown by the scale bar below the images. The blue circle represents the 1σ positional error circle determined by gtfindsrc. Various TeV emission components of HESS J1745-303 (regions A, B, and C in Figure 1 of Aharonian et al. 2008) are illustrated by the black dashed circles. (Right) Same as Left but in the energy range of 10-20 GeV. (Hui et al. 2011)
Spectral energy distribution of HESS J1745-303 as observed by Fermi LAT and H.E.S.S. The H.E.S.S. spectrum is for region A. The solid line represents the best-fit power-law model inferred in the joint analysis of both data sets. (Hui et al. 2011)
Test-statistic (TS) maps of 2 regions centered at the position of PSR B1957+20 (labeled by green crosses). The color scale below each pair of images is used to indicate the TS values. (Top): (i) TS map at energy > 2.7 GeV using only photons in Phase 1. (ii) Same as (i) but using only photons in Phase 2. (Middle): (i) TS map at < 2.7 GeV for Phase 2. (ii) Same as (i) but with data within full width at half maximum of the pulsation peaks removed (see text). (Bottom): Same as (Middle) but with energy > 2.7 GeV. (Wu et al. 2013, ApJL, in press)