Can Gamma-ray Observations Probe the Cosmic Infrared Background Radiation? Yoshiyuki Inoue (JAXA International Top Young ISAS/JAXA)
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1 Can Gamma-ray Observations Probe the Cosmic Infrared Background Radiation? Yoshiyuki Inoue (JAXA International Top Young ISAS/JAXA) 1
2 Cosmic Background Radiation E 2 dn/de [erg cm -2 s -1 sr -1 ] CMB Galaxies (Inoue et al. 13) Pop-III Stars (Inoue et al. 13) AGNs (All) Radio-quiet AGNs (Inoue et al. 08) Blazars (Inoue and Totani 09) Radio Galaxies (Inoue 11) Galaxies? AGNs? Photon Energy [ev] 2
3 Cosmic Gamma-ray Background Preliminary Ajello at HEM14 FSRQs (Ajello+ 12), BL Lacs (Ajello+ 14), Radio gals. (YI 11), & Starforming gals. (Ackermann+ 12)
4 Extragalactic Background Light (EBL) I [nw/m 2 /sr] 0 1 Stars Dust Madau & Pozzetti 00 (HST) Elbaz et al. 02 (ISO) Papovich et al. 04 (Spitzer) Fazio et al. 04 (Spitzer) Xu et al. 05 (GALEX) Dole et al. 06 (Spitzer) Frayer et al. 06 (Spitzer) Gardner et al. 00 (HST) Berta et al. 11 (Hershel/PEP) Wright & Reese 00 (DIRBE) Wright 04 (DIRBE) Levenson et al. 07 (DIRBE) Levenson & Wright 08 (DIRBE) Bernstein 07 (HST) Matsuoka et al. 11 (Pioneer) Matsumoto et al. 11 (IRTS) Matsuura et al. 11 (AKARI) CambrØsy et al. 01 (DIRBE) Dwek & Arendt 98 (DIRBE) Gorijian et al 00 (DIRBE) Finkbeiner et al 00 (DIRBE) Hauser et al 98 (DIRBE) Lagache et al 00 (DIRBE) Edelstein et al 00 (Voyger) Brown et al 00 (HST/STIS) Albert et al 08 (MAGIC) (X, z c )=(1.0, 0.0) (X, z c )=(50.0,.0) (X, z c )=(0.0,.0) [µm] 4 YI+ 13a
5 Gamma rays are attenuated by EBL blazar Extragalactic Background Light IACT γ VHE γ EBL e + e - 5
6 Blazars Log L (erg s -1 ) Log (νlν [erg/s]) FSRQ BL Lac Non-thermal emission from radio to gamma-ray Two peaks Synchrotron Inverse Compton Luminous blazars tend to Log E (ev) Log (Energy [ev]) Fossati+ 98, Kubo+ 98, YI & Totani 09 have lower peak energies (Fossati+ 98, Kubo+ 98)
7 EBL Constraints from Gamma Rays LAT best fit -- 1 sigma LAT best fit -- 2 sigma Franceschini et al Finke et al model C Stecker et al High Opacity Stecker et al Low Opacity Kneiske et al highuv Kneiske et al best fit Kneiske & Dole 20 Dominguez et al Gilmore et al fiducial Abdo et al. 20 ] sr ME12 exclusion region H.E.S.S. H.E.S.S. low energy H.E.S.S. full dataset H.E.S.S. high energy H.E.S.S. contour (sys + stat ) low full high Direct measurements τ γ γ 1 Fermi [ nw m F λ λ -1 z~1.0 z Galaxy counts 2 Energy [GeV] Ackermann + 13 Fermi and H.E.S.S. derived the EBL opacity or intensity using the combined spectra of blazars (see also Gong & Cooray 13, Dominguez + 13). Inconsistent with the NIR EBL excess. They assume simple log-parabola or power-law spectra. 7 1 λ [ µm ] Abramowski + 13 ig. 5. Flux density of the extragalactic background light versus wave-
8 Dark Energy & Gamma rays? Gamma-ray attenuation (This work) Cosmic γ-ray horizon, E0 [TeV] 1 Ackermann+ 12 Domínguez+ 13 h =0.30 h =0.40 h =0.50 h =0.60 h =0.70 h =0.80 h =0.90 h =1.00 ecmb+bao+cepheids+sne (Hinshaw et al. 2013) Planck+WP+highL+BAO (Ade et al. 2013) High-redshift galaxy clusters (Bonamente et al. 2006) Type Ia supernova (Riess et al. 2011) Gravitational lensing (Suyu et al. 2012) CMB+BAO (Anderson et al. 2012) Extragalactic HII (Chávez et al. 2012) CMB (Hinshaw et al. 2013) 0.1 Galaxy clustering (Chuang et al. 2013) Redshift Derive the cosmic expansion rate using gamma-ray horizon. total uncertainties (statistical plus systematic, added in quadrature) are shown with lighter red. The combined value presented by Hinshaw et al. (2012) is Future data may allow to constrain cosmological parameters. Dominguez & Prada 13 Cepheids (Freedman et al. 2012) H 0 [km s 1 Mpc 1 ] Dominguez & Prada 13 Figure 2. The Hubble constant H 0 derived from different methodologies. The measurement presented in this work is shown with a red star. For this measurement, the statistical uncertainties are shown with darker red, whereas the shown with a blue hexagon, which includes CMB data from WMAP9 plusthe ground-based SPT and ACT (extended CMB or ecmb), BAO, and Cepheids plus SNe measurements. The CMB+BAO measurement by Anderson et al. (2012) includes CMB data from WMAP7 and BAO from the Sloan Digital Sky Survey-II luminous red galaxy sample plus data from the Baryon Oscillation Spectroscopic Survey (BOSS). The results from the Planck Space Telescope combined with WMAP polarization low-multipole likelihood (WP) plus highresolution CMB data (highl and BAO; Ade et al. 2013) areshownwitha green square. As a reference, a shaded region is showing the H 0 value from the Cepheids distance ladder. (A color version of this figure is available in the online journal.)
9 Spectra Assumption Log-parabola (+ exp. cutoff) Single power-law (+ exp. cutoff) SSC
10 >0 GeV Gamma Rays from z=1.1 & z>0.6 PKS at z=1.1 PKS at z > Observed EBL corrected (Franceschini et al. 2008) EBL corrected (Inoue et al. 2013) Broken PL model Contemporaneous Fermi LAT from Acciari et al. 20 Contemporaneous Fermi LAT Power-law Fit from Acciari et al. 20 VERITAS Observed VHE Spectrum from Acciari et al. 20 E 2 dn/de [erg cm -2 s -1 ] - (Jy Hz) νf ν z= Absorption-corrected Spectrum using Doming uez et al z= Absorption-corrected Spectrum using Gilmore et al z=1.2 Absorption-corrected Spectrum using Dominguez et al Fermi 11 Fermi + VERITAS Energy [GeV] Tanaka, YI, Energy (GeV) Furniss Distant very high energy (VHE) sources show spectral hardening.
11 Is VHE Spectral Hardening Universal? E 2 dn/de [TeV/cm 2 /s] -9 - H z = ES z = S z = 0.31 RX J z = RBS 0413 z = 0.19 Spectra of blazars at z > 0.15 show hardening from a few hundred GeV. 1ES z = ES z = ES z = ES z = Energy [TeV] 4C z = Energy [TeV] 3C 66A z = Energy [TeV] 3C 279 z = Energy [TeV] YI+ 13a 11 Γ z z Essey Γ & Kusenko = Γ 12Γ
12 Secondary Gamma Rays? Stochastic Acceleration? KUV (z=0.61) Secondary Gamma Rays E 2 F E [erg cm -2 s -1 ] γ-induced (low IR) γ-induced (best fit) CR-induced (low IR) CR-induced (best fit) Becherini et al. (2012) H.E.S.S. I CTA 1ES (z=0.1396) Stochastic Acc. log vf 2 v [erg.sec.cm2 ] F v v 1/3 1ES (z=0.1396) E 2 Exp[-(E/E c ) 3 ] H.E.S.S. low level EBL - E 2 Exp[-E/E c ] H.E.S.S. high level EBL SWIFT -.5 F v v 1/ E [ev] Takami log v [Hz] = Lefa+ 11 Secondary gamma rays from cosmic rays along line of sight (Essey & Kusenko, Essey+, Essey+ 11, Murase+ 12, Takami+ 13) Stochastic acceleration can generate hard electron spectra (Stawarz & Petrosian 08, Lefa+ 11, Asano+ 14). Lepto-hadronic scenario (Inoue-san s talk). 12
13 Direct Measurement of EBL 0 ZE CMB Surface brightness I ν [MJy/sr] ZL DGL SL ISD wavelength [µm] 0 00 Matsuura+ 11 Foreground: Zodiacal light, Diffuse galactic light, Star light.
14 Direct Measurement of EBL Pioneer /11 IRTS AKARI Matsuoka + 11 Tsumura + 13 Pioneer /11 measurements are consistent with galaxy counts. Recent AKARI measurements are consistent with IRTS. EBL peak at near infrared? 14
15 NIR Sky Fluctuation Figure 8. Coherence, Cn4 (Pn4 (q) Pn4 (q))/(pn (q)p4 (q)), for 1 4 (blue) and 2 4 (red) for EGS (left) and UDS!(right) fields. Open sym where Pn4 < 0. The relative statistical uncertainties on the coherence resulting from cosmic variance are given by 12/Nq which is shown valid at small C when all the power spectra can be assumed independent. With Nq plotted in Figure 1 this uncertainty is of the order of 0 The Astrophysical Journal, 742:124 (11pp), 2011 December 1 Matsumoto et al. in the EGS field. The Astrophysical Journal, 742:124 (11pp), 2011 December 1 (A color version of this figure is available in the online journal.) Matsumoto + 11 Kashlinsky+ 12 Matsumoto + 11 ) Figure 7.and Spectrum of the average fluctuation large anglesblack (0 350 Figure 9. Field-averaged CIB fluctuations at 3.6 µm (left), 4.5 µm (middle), the cross-correlation poweratspectrum. solid line (shown by filled circles) is compared with the Spitzer results (open squares). The remaining known galaxies from Sullivan et al. (2007) who state that normal galaxies at Vega magnitudes from 22.5 to 26 can fit the observe open circles represent the spectrum of the correlating component normalized to (That claim, which also appears in the comments to their, pre-print posting, is contradicted by their own Figure 8 which shows the the 2.4 µm band. The solid line indicates a Rayleigh Jeans spectrum ( λ 3 ), cle KAMM1 measurements.) Because Sullivan et al. (2007) present their results only for 3.6 µm sources, their model is displayed only while the dotted line indicates the spectrum in Figure 20 of Fernandez et al. in th (20). Thethe vertical bars show error. show the residual fluctuations from Helgason et al. (2012), after reconstructing near-ir CIB1σfluctuations of known galaxies at both 3 of multiband galaxy luminosity function (LF) data. The shaded regions correspond to the high and low faint end of the LF data. At 3.6 µ the black solid line although Helgason et al. find, on average, slightly lower levels than Sullivan et al. (2007). The dashed line shows the 3.6 µm the regression leads to PSN = 57.5 njy nw m 2 sr 1 (or nw2 m 4 sr 1 ) and at 4.5 µm the shot-noise levels are PSN (or nw2 m 4 sr 1 ). Since the shot noise can be expressed as PSN SFCIB (>m0 ), it is presented in both sets of units. Blue the high-z ΛCDM (toy)-model processed through the mask of each field and then averaged as described in Appendix B. It leads to the A5 = 0.07(0.05) nw m 2 sr 1 at 3.6(4.5) µm. The thick solid red line shows the sum of the three components. (A color version of this figure is available in the online journal.) AKARI & Spitzer reported NIR background fluctuation at 2.4, 3.2, 3.6, 4.1 and 4.5 um (Kashlinsky+ 05, 07, 12, Matsumoto+ 11, Cooray+ 12) % of CIB fluctuation is correlated with CXB (Cappelluti+ 13). Figure 3 shows that within the statistical uncertainties the produced by the discreteness of the rem fields in this study have the same power spectrum of the sourceisotropy of the measured signal, which is fu subtracted fluctuations. Therefore, we averaged the two sets Appendix A for five additional fields from -3 spectrum describing the of results to obtain an overall power ments, is consistent with it being of cos (Matsumoto+ 11, Cooray+ 12) CIB. The averages were weighted with the number of Fourier the same shot-noise level, the measured elements in each field as described above. The results of the CIB agreement with our measurements at five diameter circle centered on each pixel. The lower panel shows smoothed Figure 6. Upper panel shows smoothed sky maps obtained by averaging pixels within a 50 fluctuations after averaging over (KAMM1 2) at smaller angular scales (! 15the individual fields are shown ark maps obtained by the same procedure for the dark maps. The color scales shown in the bar below each map are chosen such that sky maps and dark maps have in Figure 9. The figure indicates the presence of significant This section discusses the constraints The angular power spectrum at large scales is close to the shape of a Rayleigh-Jeans spectrum, λ
16 Can we explain the NIR EBL excess in spectrum and fluctuation? No. ] Extragalactic Background Light Spectrum with AKARI IRC 5 Figure 2. Amplitude maps of the two-dimensional fluctuation spectra, [q 2 P2 (q)/(2π )]1/2, in Fourier space. The results for the 2.4, 3.2, and 4.1 µm band are shown from the left to the right. The grayscale bars below each map indicate amplitudes of the fluctuation in units of nw m 2 sr 1. AKARI IRTS AKARI Matsumoto + 11 Figure 3. Upper panel shows the one-dimensional fluctuation spectra, [q 2 P2 /(2π )]1/2 in units of nw m 2 sr 1, obtained by two-dimensional Fourier analysis as a function of angular scale (2π )/q. Graphs correspond to the 2.4, 3.2, and 4.1 µm bands from left to right. Filled circles and open triangles show the fluctuation spectra for sky and dark maps, respectively. The lower panel shows the fluctuation spectra of the sky after subtracting those of dark maps in quadrature. The straight lines fluctuation spectra of shot noise due to unresolvedfrom faint galaxies. Allincluding error bars represent 1σ error. showindicate EBLtheby various direct photometry space Tsumura + 13 Fig. 4. Spectrum of EBL and integrated light of galaxies. Filled plots this study, and open plots shows the integrated light of galaxies by deep observations. Horizontal bars show the band widths of results taken as sequence alternating time, observed while in case B the wide-band data. Solid curve shows a model spectrum of the integrated light of agalaxies based onin the evolution of thefor both subsets are consistent with those of the stacked dark maps. This indicates that the observed structure is indeed to the earlier curve and latershows halves a of scaled our set. version rest-frame K-band galaxy luminosity function up to redshift 4 (Domı nguez subsets et al. correspond 2011), and broken of present in the original images and is of celestial origin. For both cases, we obtained two stacked images, F1 and F2, by it in case of AKARI s detection limit of point sources (mk = 19). We also examined the impact of masking on the fluctuation applying the same procedure as the one described previously in spectra, since 53% of all pixels are masked. We constructed this section. The fluctuation spectra of the difference between a common mask that includes all pixels masked in any of three twobe stacked images arealready, shown in Figure Cases A and must detected if it4. exists. An isotropic his correlation to the higher Galactic latitude regions in Earth these B are shown as squares and asterisks, respectively, while the anotherbands. The fraction of remaining pixels in images ur method. However, this assumption is obviously too diffuse background from the Oort cloud could be wavelength with the common mask applied is 32%. We again performed fluctuation spectra of the dark maps are shown by triangles. The A component other than galaxies should significantly contribute to the NIR EBL. imple. For example, UV radiation field at high Galactic atitude is weaker than that at Galactic plane (Seon et l. 2011), therefore the PAH molecules are less excited at candidate. However, the very blue spectrum toward 1 µm cannot be generated by thermal emission from very 4 cold dust (<30 K) at the Oort cloud. Scattered sunlight
17 First stars? Lyman alpha photons from z~ will redshifted to ~1 um at z=0. We might see the light for first stars. But, we need very high first star formation rate density. Fernandez & Komatsu Fernandez & Komatsu 06
18 Reionization Constraints YI+ 13a Neutral Hydrogen Fraction YI+ 13a Electron Thomson scattering opacity Ionizing photon emissivity of first stars can not violate these observed reionization data. 18
19 Constraints on First Stars Cosmic Star Formation Rate Density [M sun /yr/mpc 3 ] Fernandez & Komatsu 06 Raue, Kneiske, & Mazin 09 Gilmore 12 C = 3.0, f esc = 0.2 C = 3.0, f esc = 0.5 C = 1.0, f esc = 0.2 Bromm & Loeb 06 Trenti & Stiavelli 09 de Souza, Yoshida, & Ioka Redshift z YI+ 14 Combining reionization and distant gamma-ray data (E<0 GeV). The required first star formation rate density is inconsistent with reionization data (e.g. Madau & Silk 05; YI+ 14) 19
20 LETTER RESEARCH Intracluster Halo Stars? a l 2 C l /2π (nw m 2 sr 1 ) 2 b π/l (arcmin) IHL 1-halo 2-halo Shot noise l 3.6 μm Low-z z > 6 2π/l (arcmin) Stars stripped from host galaxies by major mergers. Intrahalo stars may create a fluctuation peak at l~00. Is this population already taken into account in galaxy counts? 0 1 Ref. 14 l 2 C l /2π (nw m 2 sr 1 ) μm f IHL 1 2 Ref. 13 Ref. 25 This study M31 MW l Cooray μm Halo mass (M/M ) Cooray+ 12
21 Summary Gamma-ray observations constrain EBL with various techniques. But, VHE distant sources show unexpected spectral hardening. It may not be straightforward to constrain EBL further through gamma-ray observations of blazars. Direct EBL measurement is hampered by foreground emission (x~0 times higher flux). Another component appears in angular power spectrum. 21
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