Sources of GeV Photons and the Fermi Results

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1 Sources of GeV Photons and the Fermi Results 1. GeV instrumentation and the GeV sky with the Fermi Gamma-ray Space Telescope 2. First Fermi Catalog of Gamma Ray Sources and the Fermi Pulsar Catalog 3. First Fermi AGN Catalog 4. Relativistic jet physics and blazars 5. γ rays from cosmic rays in the Galaxy 6. γ rays from star-forming galaxies and clusters of galaxies, and the diffuse extragalactic γ- ray background 7. Microquasars, radio galaxies, and the extragalactic background light 8. Fermi Observations of Gamma Ray Bursts 9. Fermi acceleration, ultra-high energy cosmic rays, and Fermi Thanks to L. Guillemot, S. Digel Dermer Saas-Fee Lecture March

2 Survey of Fermi Sources and the Fermi AGN and Pulsar Catalogs 1. 1FGL: the first Fermi Catalog of Gamma-Ray Sources 2. Pulsar Catalog The Fermi-LAT Collaboration 2010, arxiv: Abdo et al., 2010, ApJS, in press, arxiv: First Large Area Telescope AGN Catalog: 1LAC Abdo, et al. 2010, ApJ, submitted, arxiv: (next lecture) Dermer Saas-Fee Lecture March

3 One Year Catalog: 1FGL Sources/ Source Classes Detected with Fermi Sun, Moon, Earth 3 High Mass X-ray Binaries Rotation-powered and millisecond pulsars Supernova remnants Globular clusters > 600 blazars At least 11 Radio Galaxies Dozens of other AGNs 3 Starburst Galaxies Fermi Fermi observations of the of Quiet the Moon Sun Orlando, Giglietto, E., Giglietto, N., for N., the for Fermi the Fermi Large Area Large Telescope Area Telescope Collaboration Collaboration 2009, arxiv: , arxiv: Dermer Saas-Fee Lecture March

4 Animation of >1 GeV Fermi 1 year sky Dermer Saas-Fee Lecture March

5 First Fermi Catalog 11 months of data 100 MeV to 100 GeV, 23.3 Ms livetime 10.6 M events over the whole sky after selection Improved diffuse model (distributed with the data) and calibration with respect to 0FGL Very uniform exposure (factor 1.25 between north and south) Detection based on integrated data (not on flares) 1451 Sources, TS > 25 (>~4σ) Improved localization AGN catalog, drawn from sources above 10 latitude Pulsar catalog, drawn from all pulsed detections of both radio and γ-ray pulsars GRB catalog, GBM and LAT detections Dermer Saas-Fee Lecture March

6 Fermi >200 MeV 1 Year Sky Map Dermer Saas-Fee Lecture March

7 Sky Map of 1FGL Sources Dermer Saas-Fee Lecture March

8 LAT 1FGL Source Classes Associations Firm identifications (in parentheses) based on temporal variability or source morphology Dermer Saas-Fee Lecture March

9 The flux limit is not well defined depends on source spectra and diffuse background intensity Analytical approximation for highlatitude sky works well Lower envelope is from energy dependence of the PSF width Confusion (overlapping PSFs) reduces sensitivity for the softer sources N.B. Spectra are only approximately power-law Flux limits at low latitudes are factors of ~few greater Flux Limit vs. Spectral Hardness: F(>100 MeV) Power-law fit 10-9 cm -2 s -1 Distribution of flux >1 GeV All 1FGL sources b > 10 Dermer Saas-Fee Lecture March

10 Pulsars with Fermi Pulsars: rapidly rotating, highly magnetized neutrons stars, born in supernova explosions of massive stars or accretion-induced collapse of white dwarfs. Typically, M ~ 1.4 M sun and R ~ 10 km A dense plasma is found in the closed-field lines co-rotating with the star. The magnetosphere extends to the light cylinder, where the rotation reaches the speed of light. Emission (radio, optical, X-ray ) can be produced in beams around the pulsar, which acts like a cosmic light-house, probably accelerated on field-lines open to the light cylinder. ~ 1900 pulsars known today, most in radio Dermer Saas-Fee Lecture March

11 The Pulsing γ-ray Sky Pulses at 1/10 th true rate (as of Jan 2009) Dermer Saas-Fee Lecture March

12 Pulsar Properties from Observations: Elementary Concepts Observations give Characteristic age Light cylinder radius: Theory gives M ns, R ns Ω=2π/P Magnetic field at the neutron star surface (equating rotational spindown energy with magnetic dipole radiation): Goldreich-Julian density for a force-free magnetosphere: Dermer Saas-Fee Lecture March

13 Gamma-ray pulsars before Fermi Brightest sources in the 100 MeV GeV sky Before Fermi and AGILE: 6 detections by EGRET, 1 by COMPTEL (all normal energetic pulsars; Geminga lacks radio counterpart), + a few marginal detections. MeV-GeV emission: dominates energy budget No TeV detections Dermer Saas-Fee Lecture March

14 Emission geometry and γ-ray pulsar properties Different Some ques)ons theoretical Fermi models can answer: try to explain the observed gamma-ray emission. Are all the gamma- ray pulsars consistent with T h e y a s s u m e d i f f e r e n t o r i g i n i n t h e magnetosphere one type of emission => different model? emission geometry (two main models: outer gap and polar cap). How do the gamma- ray pulsars compare to the radio pulsars in terms of physical proper<es Pulse such as profile age, depends magne<c on: field, spin- down α: luminosity, angle between and other magnetic parameters? and rotation axis β: angle between line-of-sight and magnetic axis Are the trends suggested by the CGRO pulsars confirmed by the LAT gamma- ray Different emission patterns are expected (number of pulsars? peaks, separation, radio/gamma lag, ratio of radio-loud/radio-quiet). Which of the LAT pulsars are associated with SNRs, PWNe, uniden<fied EGRET sources, or TeV sources? Curvature radiation, (coherent) synchrotron radiation, Compton radiation What is the contribu<on of gamma- ray pulsars to the diffuse galac<c emission? Gamma-ray observations can help disentangle the geometry of pulsars. Dermer Saas-Fee Lecture March

15 Discovering pulsars with the Fermi LAT Two different approaches: Blind search of the rotational parameters in the gamma-ray data (new pulsars) Period folding Time-differencing techniques Using rotational parameters obtained in radio or X rays (known pulsars) First blind search detec<on was a 317 ms pulsar in shell SNR CTA1, coincident with uniden<fied X- ray and 3EG J γ- ray sources. (1420 MHz radio map) (Abdo et al., Science 322, 1218, 2008) Spin- down power: erg s - 1 Pulsar s inferred age: 14,000 yr (consistent with SNR age) Dermer Saas-Fee Lecture March

16 Gamma-ray selected (blind-search) pulsars Where to search? Geminga candidates: CTA1, 3EG J («next Geminga»), compact objects Unidentified Fermi sources. 16 of the first 46 Fermi pulsars were unidentified EGRET sources, A`er 4 months of data taking, 16 pulsars have been found with the same technique (Abdo et al., Science 325, 840, 2009) Dermer Saas-Fee Lecture March

17 EGRET pulsars with Fermi EGRET pulsars generally are prime targets for spectral analyses with unprecedented details, because of their brightness. Vela: brightest source in the >100 MeV γ- ray sky Varia<on seen in spectral proper<es across the rota<on. Spectral index and cutoff energy varia<ons are thought to be due to emission al<tude changes with energy In general, pulsar spectra are consistent with simple- exponen<al cutoffs, not super- exponen<al cutoffs, indica<ve of absence of magne<c pair ahenua<on. Dermer Saas-Fee Lecture March

18 Young radio-loud pulsars Fermi detected a number of young radioloud gamma-ray pulsars, all highly energetic (Ė > erg/s). Many are seen in unidentified EGRET s o u r c e s : 3 E G J , 3 E G J , 3EG J , 3EG J , PSR J PSR (Abdo J et al., ApJL 695, 72, 2009) (Weltevrede et al., ApJ 2009 submiied) PSR J (Abdo et al., ApJ 700, 1059, 2009) PSR J & J PSR J (Abdo et (Abdo al., ApJ et 2009 al., ApJL accepted) 699, 102, 2009) Dermer Saas-Fee Lecture March

19 Pulse Profiles and Spectra The gamma-ray profiles typically are twopeaked; the first one lagging the radio by 0.1 to 0.2 (with a few exceptions, e.g. J ). Gamma rays Radio The Two-Pole Caustic (TPC) or the Outer Gap (OG) models generally provide good fits to the observed profiles. Polar Cap emission remains plausible for some pulsars. OG (green) and TPC (magenta) fits to J s light curve (Venter et al. ApJ, 2009, accepted) Spectra are consistent with exponentially cutoff power-laws, with cutoff energies below 10 GeV. Cutoff energy vs. B LC for the 46 catalog PSRs Dermer Saas-Fee Lecture March

20 Radio-loud millisecond pulsars The LAT detected pulsed gammaray emission from J , making it the first firm detection of an MSP in gamma rays (Abdo et al., ApJ 699, 1171, 2009) After 9 months of data taking, the LAT had detected 8 gamma-ray MSPs (Abdo et al. Science 325, 848, 2009) For the first time, a population of gamma-ray MSPs has been observed. Dermer Saas-Fee Lecture March

21 Fermi Detection of the Globular Cluster 47 Tucanae >200 MeV, 17σ from 47 Tuc γ-ray spectral shape consistent with large populations of ms pulsars Globular clusters contain old, ~1010 yr, stellar populations Number of LMXBs correlated with stellar encounter rate With typical <~ erg s-1 in γrays, require ~20-40 ms pulsars Abdo, A. A., et al. 2009, Science, 325, 845 Lγ erg s cts > 200 MeV Dermer Saas-Fee Lecture March

22 Spin-down Ages and Luminosities As for EGRET, the detected pulsars are relatively close and highly energetic. Detected pulsars also have the highest values of magnetic field at the light cylinder, B LC. Both detected normal PSRs and MSPs have comparable B LC values. Similar emission mechanisms operating? B LC vs. characterisyc age for the catalog PSRs Luminosities are affected by distance uncertainties. However, the luminosity seems to grow with spin-down energy; with a L Ė at low Ė, L Ė at high Ė. Gamma- ray luminosity vs. spin- down energy for the catalog PSRs Dermer Saas-Fee Lecture March

23 Comprehensive, uniform presentation of 46 pulsars detected by the LAT using the first 6 months of LAT data (63 in 1FGL) Of the 46, 16 resulted from blind searches, and 24 were discovered using ephemerides from radio monitoring, including 8 MSPs Light curves (with tabulated peak phases), spectral fits, log N-log S Dermer Saas-Fee Lecture March

24 Fermi Pulsar Catalog In addition to the search for new pulsars, 762 known pulsars with ephemerides were searched for pulsations in nine months of data. 46 pulsars were detected, and an additional 17 found between Fermi pulsar catalog and 1FGL) (radio, optical, X-ray pulsar catalog) Abdo et al., ApJS, 2010, in press, arxiv: Dermer Saas-Fee Lecture March

25 1FGL Catalog Highlights 1451 sources above 4.1σ significance threshold Typical 95% error radius is 10. Absolute accuracy is <1 241 sources show evidence of variability About half the sources are associated positionally, mostly with blazars (~600) and pulsars (~60) Other classes of sources exist in small numbers (XRB, PWN, SNR, starbursts, globular clusters, radio galaxies, narrow-line Seyferts) Uncertainties due to the diffuse model, particularly in the Galactic ridge, should be kept in mind for low-latitude and local cloud studies The Catalog is an analysis product but also a useful input for many other studies with LAT data Dermer Saas-Fee Lecture March

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