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Searching for Pulsars in Unassociated Fermi-LAT Sources

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Searching for Pulsars in Unassociated Fermi-LAT Sources Searching for Pulsars in Unassociated Fermi -LAT sources Hung Kit (Jason) Wu Searching for Pulsars in Unassociated Fermi -LAT sources Dissertation zur Erlangung des Doktorgrades (Dr. rer. nat.) der Mathematisch-Naturwissenschaftlichen Fakultät der Rheinischen Friedrich–Wilhelms–Universität Bonn vorgelegt von Hung Kit (Jason) Wu Bonn, 2017 Angefertigt mit Genehmigung der Mathematisch-Naturwissenschaftlichen Fakultät der Rheinischen Friedrich–Wilhelms–Universität Bonn 1. Referent: Prof. Dr. M. Kramer 2. Referent: Prof. Dr. N. Langer Tag der Promotion: 09.04.2018 Erscheinungsjahr: 2018 Diese Dissertation ist auf dem Hochschulschriftenserver der ULB Bonn unter http://hss.ulb.uni-bonn.de/diss_online elektronisch publiziert RHEINISCHE FRIEDRICH–WILHELMS–UNIVERSITÄT BONN Abstract by Hung Kit (Jason) Wu for the degree of Doctor rerum naturalium Pulsars have always been under the γ-ray spotlight since the birth of γ-ray as- tronomy. They were the first sources that were firmly established as γ-ray sources in the 70s. Since then, pulsars have been the prime suspect of unassociated γ-ray sources in our Galaxy. The Large Area Telescope (LAT) is the game changer of γ- ray astronomy, on-board the Fermi Gamma-ray Space Telescope which launched in 2008, has increase the known population of γ-ray by over a factor of 30 in just 8 years. It enabled the discoveries of pulsars in different types through their γ-ray pulsations, including a large number of millisecond pulsars, which were originally thought to be weak in γ-rays. Many of the young γ-ray pulsars discovered have not yet been detected in subsequent radio searches, like the famous Geminga pul- sar. These “radio-quiet” γ-ray pulsars population can only be accessed through blind periodicity searches in γ-rays. Therefore, γ-ray observations is the only way to complete the radio-quiet part of the Galactic pulsar population. This thesis describe the most recent major blind search survey of γ-ray pulsar – Einstein@Home γ-ray pulsar survey. Firstly, technique using machine learn- ing were used in identifying viable unassociated γ-ray sources for blind searches. This algorithm incorporate spectral, temporal behaviour and γ-ray flux informa- tion of individual γ-ray sources to divide them into different clusters. Secondly, LAT photons associated with these sources were weighted according to the spec- tral result to improve the sensitivity of subsequent blind searches. γ-ray sources selected for the blind-search survey was performed on the distributed volunteer computing system Einstein@Home using the multi-stages semi-coherent tech- nique, which is optimized for the long duration LAT dataset. This resulted in the discovery of seventeen isolated γ-ray pulsars. Follow-up multi-wavelength analysis reveals the new discoveries are mostly similar with the existing γ-ray pulsar population. However, temporal behaviours of several pulsars discovered in this survey are peculiar. This includes a young glitching pulsar PSR J1906+0722; the youngest radio-quiet γ-ray pulsar ever found PSR J1208 6238, its high magnetic field strength with its young age enable the measurement− of its braking index, which is the only measurement for radio-quiet γ-ray pulsar; the discovery of the first two isolated millisecond pulsars PSRs J1035 6720 & J1744 7619 from γ-ray blind search, one of which remained radio quiet− despite the− deepest searches conducted by the Parkes radio telescope. Utilizing Effelsberg’s Ultra-Broad-Band receiver, currently under commission, originally designed for precision pulsar timing, 54 unassociated γ-ray sources were observed to explore the possibility of using wide band receiver for simultaneous pulsar searching observation in multiple radio bands. Simulations of the expected discovery yield suggested that less than one pulsar is expected to be found by random chance. Flux densities upper limits were present for all observations and the reasons of non-detection were also discussed. This thesis is concluded by the summary of the completed blind search survey, current status of ongoing and upcoming blind search γ-ray pulsar projects, and the impact of the new collection of γ-ray pulsars to the current pulsar population. To humanity... Each piece, or part, of the whole nature is always an approximation to the complete truth, or the complete truth so far as we know it. In fact, everything we know is only some kind of approximation, because we know that we do not know all the laws as yet. Therefore, things must be learned only to be unlearned again or, more likely, to be corrected. The test of all knowledge is experiment. Experiment is the sole judge of scientific “truth”. Richard Feynman The Feynman Lectures, Introduction Contents 1 Pulsars Astrophysics1 1.1 Introduction..................................2 1.2 Characteristics of pulsars..........................3 1.2.1 Spin period and spin-period derivative...............3 1.2.2 Rotational energy loss........................3 1.2.3 Magnetic field.............................4 1.2.4 Magnetic braking...........................6 1.2.5 Age estimate.............................6 1.2.6 Dispersion...............................7 1.3 Pulsar population...............................9 1.3.1 The P P_ diagram.........................9 − 1.3.2 Canonical pulsars...........................9 1.3.3 Millisecond pulsars (MSPs)..................... 11 1.3.4 Mildly-recycled pulsars........................ 11 1.4 Pulsars in γ-ray................................ 12 1.4.1 Fermi-LAT.............................. 12 1.4.2 Early discoveries from Fermi-LAT................. 12 1.4.3 γ-ray pulsar population....................... 14 1.4.4 Blind searches with Fermi-LAT data................ 17 1.4.5 γ-ray pulsar candidate........................ 18 1.4.6 Radio-quiet fraction......................... 19 1.5 Pulsar emission model............................ 19 1.5.1 Magnetosphere............................ 19 1.5.2 Radiation Processes......................... 20 1.5.3 Radio emission............................ 21 1.5.4 Models for γ-ray emission...................... 21 1.5.4.1 Slot gap and Two-pole Caustic models.......... 23 1.5.4.2 Outer gap model...................... 23 1.5.4.3 Pair-starved Polar Cap model............... 25 1.5.4.4 Striped Wind model.................... 25 1.5.5 Mapping Emission Geometry.................... 25 1.6 Scope and structure of this thesis...................... 26 2 γ-ray “informatics” 29 2.1 Fermi LAT data challenge.......................... 29 2.1.1 Maximum-Likelihood Analysis of γ-ray data............ 30 2.1.2 Fermi Science-tools and the Pointlike package........... 33 2.2 Fermi LAT Source Catalogs (0; 1; 2; 3-FGL)................ 35 2.3 Selecting pulsar candidates......................... 35 2.4 Analysis pipeline............................... 40 3 Blind Search Techiques in Radio and Gamma-ray 43 3.1 Periodicity search in radio.......................... 43 3.1.1 Data acquisition........................... 44 3.1.2 Radio Frequency Interference (RFI) removal............ 44 3.1.3 De-dispersion............................. 46 3.1.4 Periodicity search........................... 46 3.1.5 Pulsar candidate........................... 47 3.1.6 Folding and Confirmation...................... 47 3.2 Periodicity search in γ-ray.......................... 48 3.2.1 Photon weighting technique..................... 48 3.2.2 Semi-coherent stage......................... 51 3.2.3 Coherent follow-up.......................... 51 3.2.4 Higher signal harmonics....................... 53 3.3 Summary................................... 53 4 The Einstein @ Home Gamma-Ray Pulsar Survey : 13 new discover- ies 57 4.1 Introduction.................................. 58 4.2 Source selection................................ 60 4.2.1 3FGL catalog............................. 60 4.2.2 Pulsar candidate classification.................... 60 4.3 Data preparation............................... 61 4.3.1 The spectral analysis pipeline.................... 61 4.3.2 Relocalization............................. 63 4.3.3 Search summary........................... 63 4.4 Follow-up Analysis.............................. 64 4.4.1 Spectral Analysis........................... 64 4.4.2 Radio counterpart searches..................... 68 4.4.3 Pulse profile modeling........................ 70 4.4.4 Luminosity, distance and gamma-ray efficiency.......... 71 4.4.5 X-ray counterpart searches..................... 72 4.5 Discussion................................... 74 4.6 Conclusions.................................. 76 5 Discovery Highlights From Einstein@Home 89 5.1 A γ-ray Pulsar With Giant Glitch – PSR J1906+0722.......... 90 5.1.1 Pulsar properties........................... 90 5.1.2 Implications.............................. 94 5.2 A Radio Quiet γ-ray pulsar with a measurable Braking Index – PSR J1208 6238.................................. 95 − 5.2.1 Pulsar properties........................... 95 5.2.2 Implications.............................. 95 5.3 Millisecond Pulsars found in blind search.................. 101 5.3.1 Pulsars properties.......................... 101 5.3.2 Implications.............................. 103 5.4 Summary................................... 103 6 A Radio Pulsar Survey at Effelsberg using the Ultra Broad-Band (UBB) Receiver 107 6.1 Introduction.................................. 107 6.2 The Ultra Board Band receiver....................... 108 6.3 Observations and Analysis.......................... 108 6.4 Sensitivity................................... 110 6.5 Simulations.................................
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