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THE FERMI HAZE: A GAMMA-RAY COUNTERPART TO THE MICROWAVE HAZE
Open accessAbstract
The Fermi Gamma-ray Space Telescope reveals a diffuse inverse Compton (IC) signal in the inner Galaxy with a similar spatial morphology to the microwave haze observed by WMAP, supporting the synchrotron interpretation of the microwave signal. Using spatial templates, we regress out π 0 gammas, as well as IC and bremsstrahlung components associated with known soft-synchrotron counterparts. We find a significant gamma-ray excess toward the Galactic center with a spectrum that is significantly harder than other sky components and is most consistent with IC from a hard population of electrons. The morphology and spectrum are consistent with it being the IC counterpart to the electrons which generate the microwave haze seen at WMAP frequencies. In addition, the implied electron spectrum is hard; electrons accelerated in supernova shocks in the disk which then diffuse a few kpc to the haze region would have a softer spectrum. We describe the full-sky Fermi maps used in this analysis and make them available for download.
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“The presence of a large-scale outflow from the center of our own Galaxy was confirmed after the discovery of two large ( ∼ 8 -10 kpc) γ -ray bubbles using the Fermi-LAT telescope.”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Dobler et al. 2010
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Cites
Schlegel, D. J., Finkbeiner, D. P., & Davis, M. (1998) · The Astrophysical Journal · doi:10.1086/305772 · Cited by 15,126
Self-citationCosmic-Ray Propagation and Interactions in the Galaxy
Strong, A. W., Moskalenko, I. V., & Ptuskin, V. S. (2007) · Annual Review of Nuclear and Particle Science · doi:10.1146/annurev.nucl.57.090506.123011 · Cited by 1,251 · cited 1×
“A schematic of the relative importance of these emission mechanisms in the Galactic plane (|ℓ| ≤ 30, |b| ≤ 5) generated by the GALPROP code, version 50p (Strong et al. 2000; Porter & Strong 2005; Strong et al. 2007) is shown in Figure 2.”
MethodHigh-mass X-ray binaries as a star formation rate indicator in distant galaxies
Grimm, H. J., Гильфанов, М. Р., & Sunyaev, R. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06224.x · Cited by 676 · cited 2×
“Examining known point source populations (of AGN and X-ray binaries) generally yields spectral indices α ∼ 1.5−2.2, although at high luminosities steeper power laws with α ∼ 2.5 have been observed in flat spectrum radio quasars, and at low luminosities very shallow power laws with α ∼ 1.2 have been measured in LMXB po…”
InfluentialDiffuse Continuum Gamma Rays from the Galaxy
Strong, A. W., Moskalenko, I. V., & Reimer, O. (2000) · The Astrophysical Journal · doi:10.1086/309038 · Cited by 640 · cited 1×
“A schematic of the relative importance of these emission mechanisms in the Galactic plane (|ℓ| ≤ 30, |b| ≤ 5) generated by the GALPROP code, version 50p (Strong et al. 2000; Porter & Strong 2005; Strong et al. 2007) is shown in Figure 2.”
MethodFERMI/LARGE AREA TELESCOPE BRIGHT GAMMA-RAY SOURCE LIST
Abdo, A. A., Ackermann, M., Ajello, M., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Band, D. L., Barbiellini, G., Bastieri, D., et al. (2009) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/183/1/46 · Cited by 513 · cited 3×
“…power laws with α ∼ 2.5 have been observed in flat spectrum radio quasars, and at low luminosities very shallow power laws with α ∼ 1.2 have been measured in LMXB populations (Grimm et al. 2003; Gilfanov 2004; Kim & Fabbiano 2004; Voss & Gilfanov 2006; Padovani et al. 2007; Abdo et al. 2009a).”
BackgroundInfluentialTHE FIRST FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS
Abdo, A. A., Ackermann, M., Ajello, M., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., et al. (2010) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/187/2/460 · Cited by 463
Abdo, A. A., Ackermann, M., Ajello, M., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Baughman, B. M., et al. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/700/1/597 · Cited by 428
Low-mass X-ray binaries as a stellar mass indicator for the host galaxy
Гильфанов, М. Р. (2004) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2004.07473.x · Cited by 371 · cited 1×
“…power laws with α ∼ 2.5 have been observed in flat spectrum radio quasars, and at low luminosities very shallow power laws with α ∼ 1.2 have been measured in LMXB populations (Grimm et al. 2003; Gilfanov 2004; Kim & Fabbiano 2004; Voss & Gilfanov 2006; Padovani et al. 2007; Abdo et al. 2009a).”
InfluentialHigh-energy gamma-ray results from the second small astronomy satellite
Fichtel, C. E., Hartman, R. C., Kniffen, D. A., Thompson, D. J., Öğelman, H., Özel, M. E., Tümer, T. O., & Bignami, G. F. (1975) · The Astrophysical Journal · doi:10.1086/153590 · Cited by 357 · cited 1×
“Previous studies of high latitude gamma-ray emission have reported measurements of an excess of emission above the Galactic plane, most notably SAS2 (Fichtel et al. 1975; Kniffen & Fichtel 1981), COS-B (Strong 1984), and EGRET (Smialkowski et al. 1997; Dixon et al. 1998).”
BackgroundMicrowave Interstellar Medium Emission Observed by the Wilkinson Microwave Anisotropy Probe
Finkbeiner, D. P. (2004) · The Astrophysical Journal · doi:10.1086/423482 · Cited by 331 · cited 4×
“…which roughly matches the microwave haze (i.e., centered on the GC, roughly spherical, and about 20-40◦ in radius), we now attempt to remove the π0 emission from the maps shown in Figure 1, using the same template fitting technique used in Finkbeiner (2004a) and Dobler & Finkbeiner (2008).”
BackgroundMethodInfluentialSelf-citation
Research works printed but not linked: 3
- Haslam, 1982, A&AS, 47, 1
- Porter, 2005, ICRC (Pune), 4, 77
- Slatyer, 2010, MNRAS
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Items 101–200 of 280
Mapping Outflowing Gas in the Fermi Bubbles: A UV Absorption Survey of the Galactic Nuclear Wind*
Ashley, T., Fox, A. J., Jenkins, E. B., Wakker, B. P., Bordoloi, R., Lockman, F. J., Savage, B. D., & Karim, T. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab9ff8 · Cited by 35
TRACING THE MILKY WAY NUCLEAR WIND WITH 21 cm ATOMIC HYDROGEN EMISSION
Lockman, F. J., & McClure-Griffiths, N. M. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/826/2/215 · Cited by 34
“Evidence has come from across the electromagnetic spectrum, including extended soft X-ray emission (Snowden et al. 1997; Sofue 2000; Bland-Hawthorn & Cohen 2003), diffuse microwave excess from WMAP (Finkbeiner 2004; Dobler et al. 2010) and polarized radio continuum (Carretti et al. 2013).”
BackgroundMulti-scale feedback and feeding in the closest radio galaxy Centaurus A
McKinley, B., Tingay, S., Gaspari, M., Kraft, R., Matherne, C., Offringa, A., McDonald, M., Calzadilla, M., Veilleux, S., Shabala, S., et al. (2021) · Nature Astronomy · doi:10.1038/s41550-021-01553-3
TASI 2014 Lectures: The Hunt for Dark MatterPreprint
Gelmini, G. B. (2015) · arXiv (Cornell University) · doi:10.48550/arxiv.1502.01320 · Cited by 33
Gamma rays from the Galactic Centre region: A review
van Eldik, C. (2015) · Astroparticle Physics · doi:10.1016/j.astropartphys.2015.05.002 · Cited by 33
Large-Scale Features of the Radio Sky and a Model for Loop I
Dickinson, C. (2018) · Galaxies · doi:10.3390/galaxies6020056 · Cited by 31
“The Fermi Bubbles (FB) form a double-lobed feature detected in Fermi data at energies ∼10–500 GeV centred exactly on the GC and reaching up to b = ±55◦ [35,36].”
BackgroundGhosh, T., Banday, A. J., Jaffe, T., Dickinson, C., Davies, R. D., Davis, R., & Gorski, K. M. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.20875.x · Cited by 31
“Nevertheless, the microwave haze remains an active area of research, particularly given its possible association with a gamma-ray counterpart observed in the Fermi data (Dobler et al. 2010).”
BackgroundA HADRONIC–LEPTONIC MODEL FOR THE FERMI BUBBLES: COSMIC-RAYS IN THE GALACTIC HALO AND RADIO EMISSION
Fujita, Y., Ohira, Y., & Yamazaki, R. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/789/1/67 · Cited by 23
“The Fermi bubbles are huge gamma-ray structure detected by the Fermi gamma-ray satellite (Dobler et al. 2010; Su et al. 2010; Su & Finkbeiner 2012).”
BackgroundHigh Energy Neutrinos from the Fermi Bubbles
Lunardini, C., & Razzaque, S. (2012) · Physical Review Letters · doi:10.1103/physrevlett.108.221102 · Cited by 31
THE TRANSPORT OF COSMIC RAYS ACROSS MAGNETIC FIELDLINES
Desiati, P., & Zweibel, E. G. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/791/1/51 · Cited by 31
“The Fermi bubbles (Finkbeiner 2004; Dobler et al. 2010)—which may have been created by sporadic activity in the Galactic center—are a local example.”
BackgroundSignatures of clumpy dark matter in the global 21 cm background signal
Cumberbatch, D. T., Lattanzi, M., & Silk, J. I. (2010) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.82.103508 · Cited by 31
Fermi Bubbles under Dark Matter Scrutiny Part II: Particle Physics AnalysisPreprint
Wei-chih Huang, A., Alfredo Urbano, A., & Wei Xue, B. (2016) · Cited by 31
W -WIMP annihilation as a source of the Fermi bubbles
Anchordoqui, L. A., & Vlček, B. (2013) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.88.043513 · Cited by 30
STEADY-STATE HADRONIC GAMMA-RAY EMISSION FROM 100-MYR-OLD FERMI BUBBLES
Crocker, R. M., Bicknell, G. V., Carretti, E., Hill, A. S., & Sutherland, R. S. (2014) · The Astrophysical Journal · doi:10.1088/2041-8205/791/2/l20 · Cited by 30
“The Fermi Bubbles (Dobler et al. 2010; Su et al. 2010) are giant 1-100 GeV γ-ray structures that extend ∼7 kpc north and south from the Galactic nucleus.”
BackgroundProbing the Southern Fermi Bubble in Ultraviolet Absorption Using Distant AGNs
Karim, M. T., Fox, A. J., Jenkins, E. B., Bordoloi, R., Wakker, B. P., Savage, B. D., Lockman, F. J., Crawford, S. M., Jorgenson, R. A., & Bland-Hawthorn, J. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aac167 · Cited by 29
“Their origin and nature is an active area of observational and theoretical research (see Dobler et al. 2010; Su et al. 2010; Crocker & Aharonian 2011; Yang et al. 2012; Ackermann et al. 2014; Yang et al. 2014; Crocker et al. 2015, and references therein).”
BackgroundProbing the Outflowing Multiphase Gas ∼1 kpc below the Galactic Center
Savage, B. D., Kim, T.-S., Fox, A. J., Massa, D., Bordoloi, R., Jenkins, E. B., Lehner, N., Bland-Hawthorn, J., Lockman, F. J., Hernandez, S., et al. (2017) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aa8f4c · Cited by 28
“The spectacular γ-ray emission bubbles (Fermi bubbles), discovered by the Fermi Gamma-ray Space Telescope, extend±50° in Galactic latitude (±10 kpc) and ±20° in Galactic longitude (Dobler et al. 2010; Su et al. 2010; Crocker & Aharonian 2011; Ackermann et al. 2014).”
BackgroundDetection potential of the KM3NeT detector for high-energy neutrinos from the Fermi bubbles
Adrián-Martínez, S., Ageron, M., Aguilar, J., Aharonian, F., Aiello, S., Albert, A., Alexandri, M., Ameli, F., Anassontzis, E., Anghinolfi, M., et al. (2013) · Astroparticle Physics · doi:10.1016/j.astropartphys.2012.11.010 · Cited by 16
Gravitational collapse in one dimension
Schulz, A. E., Dehnen, W., Jungman, G., & Tremaine, S. D. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt073 · Cited by 28
“…particle dark matter (Maciejewski et al. 2011; Vogelsberger & White 2011) and for indirect detection from dark-matter annihilation near the Galactic center (Hooper et al. 2007; Dobler et al. 2010) or in halo substructure (Diemand et al. 2008; The Fermi-LAT Collaboration: M. Ackermann et al. 2011).”
BackgroundMULTI-WAVELENGTH EMISSION FROM THE FERMI BUBBLES. I. STOCHASTIC ACCELERATION FROM BACKGROUND PLASMA
Cheng, K.-S., Chernyshov, D., Dogiel, V., & Ko, C.-M. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/790/1/23 · Cited by 19
“Introduction Recent discovery of a mysterious, diffuse gamma-ray emission from the central portion of the Milky Way (Dobler et al. 2010; Su et al. 2010) which are seen as giant features (Fermi Bubbles) elongated perpendicular to the Galactic plane, was one of the marvelous discoveries in high…”
BackgroundMAGNETIC SUBSTRUCTURE IN THE NORTHERN FERMI BUBBLE REVEALED BY POLARIZED MICROWAVE EMISSION
Jones, D., Crocker, R., Reich, W., Ott, J., & Aharonian, F. (2012) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/747/1/l12 · Cited by 25
“The Bubbles’ emission has been hypothesized (Dobler et al 2010) to be produced by the same population of highly-relativistic cosmic-ray electrons which emit synchrotron radiation at tens-of-GHz frequencies and are posited to simultaneously produce & 1 GeV gamma-rays through the inverse Compton…”
BackgroundFERMIGAMMA-RAY HAZE VIA DARK MATTER AND MILLISECOND PULSARS
Malyshev, D. V., Cholis, I., & Gelfand, J. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/722/2/1939 · Cited by 25
“1On leave of absence from ITEP, Moscow, Russia, B. Cheremushkinskaya 25 2NSF Astronomy and Astrophysics Postdoctoral Fellow Recently, Dobler et al. (2010) have found evidence for a γ-ray haze in the halo around the Milky Way Galactic center (GC).”
BackgroundInfluentialSelf-citationAngelis, A. D., & Mallamaci, M. (2018) · The European Physical Journal Plus · doi:10.1140/epjp/i2018-12181-0 · Cited by 25
Cheng, K.-S., Chernyshov, D., Dogiel, V., & Ko, C.-M. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/804/2/135 · Cited by 18
“Recently, Fermi discovered two giant gamma-ray bubbles (FBs) that extend nearly 10 kpc in diameter north and south of the Galactic center (GC; see Dobler et al. 2010; Su et al. 2010; for more recent analyses,see also Hooper & Slatyer 2013; Ackermann et al. 2014; Yang et al. 2014).”
BackgroundKinematics of the Magellanic Stream and Implications for Its Ionization*
Fox, A. J., Frazer, E. M., Bland-Hawthorn, J., Wakker, B. P., Barger, K. A., & Richter, P. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab92a3 · Cited by 25
“…compelling evidence that now exists for recent (Myr-timescale) activity at the GC, including the giant γ-ray emitting Fermi Bubbles (Su et al. 2010; Dobler et al. 2010; Ackermann et al. 2014), their counterparts in X-rays (Bland-Hawthorn & Cohen 2003; Miller & Bregman 2016), microwaves…”
BackgroundTahara, M., Kataoka, J., Takeuchi, Y., Totani, T., Sofue, Y., Hiraga, J. S., Tsunemi, H., Inoue, Y., Kimura, M., Cheung, C. C., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/802/2/91 · Cited by 24
“They extend north and south centering on the Galactic center for about 5 kpc in each direction, with a longitudinal width of ∼40° (Dobler et al. 2010; Su et al. 2010; Ackermann et al. 2014).”
BackgroundFERMI BUBBLE γ-RAYS AS A RESULT OF DIFFUSIVE INJECTION OF GALACTIC COSMIC RAYS
Thoudam, S. (2013) · The Astrophysical Journal · doi:10.1088/2041-8205/778/1/l20 · Cited by 24
“…seem to suggest that the FB γ -rays (measured in the range of ∼1–100 GeV) are produced by high-energy electrons via an inverse Compton scattering process, as the same electrons can also simultaneously produce synchrotron radiations in the presence of magnetic fields (Dobler et al. 2010).”
BackgroundLinden, T., Profumo, S., & Anderson, B. (2010) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.82.063529 · Cited by 23
Cheng, K.-S., Chernyshov, D., Dogiel, V., & Ko, C.-M. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/799/1/112 · Cited by 14
“Introduction The origin of giant gamma-ray structure named as Fermi bubbles (FBs) discovered from analysis of the Fermi-LAT data (see, Dobler et al. 2010; Su et al. 2010; Ackermann et al. 2014) is still enigmatic.”
BackgroundIDENTIFYING THE RADIO BUBBLE NATURE OF THE MICROWAVE HAZE
Dobler, G. (2012) · The Astrophysical Journal · doi:10.1088/2041-8205/760/1/l8 · Cited by 23
“It is interesting to note that this spectrum of the “cap” of the bubble is somewhat softer than that found by Dobler et al. (2010) and Su et al. (2010) who include lower latitudes, in agreement with the IC scenario (since the higher energy optical and IR components of the ISRF have lower amplitude…”
BackgroundMethodResultInfluentialSelf-citationAnalyzing the gamma-ray sky with wavelets
Balaji, B., Cholis, I., Fox, P., & McDermott, S. D. (2018) · Physical Review D · doi:10.1103/physrevd.98.043009 · Cited by 16
Self-citationDiffuse galactic gamma rays at intermediate and high latitudes. I. Constraints on the ISM properties
Cholis, I., Tavakoli, M., Evoli, C., Maccione, L., & Ullio, P. (2011) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2012/05/004 · Cited by 20
Self-citationLight weakly interacting massive particles
Gelmini, G. B. (2017) · Reports on Progress in Physics · doi:10.1088/1361-6633/aa6e5c · Cited by 21
“The Haze is now considered part of the ‘Fermi bubbles’ (discovered in 2009 by Dobler et al [102, 103]), two large structures of γ-ray emission of 8 kpc in diameter each, on both sides of the galactic plane.”
BackgroundSearch for dark matter signals withFermi-LAT observation of globular clusters NGC 6388 and M 15
Feng, L., Yuan, Q., Yin, P.-F., Bi, X.-J., & Li, M. (2012) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2012/04/030 · Cited by 20
“The analysis of the Fermi -LAT data in the Galactic center region did see some excesses with respect to the background model [9, 10], however, there is no strong indication of signals from DM annihilation or decay.”
Fermi Bubble Edges: Spectrum and Diffusion Function
Keshet, U., & Gurwich, I. (2016) · The Astrophysical Journal · doi:10.3847/1538-4357/aa6936 · Cited by 17
“This scenario was revived by the discovery (Dobler et al. 2010; Su et al. 2010, henceforth S10) of two large γ-ray, so-called Fermi, bubbles (FBs), symmetrically rising far from the Milky Way plane yet morphologically connected, at least approximately and in projection, to the intermediate-scale…”
BackgroundDirect observations of the atomic-molecular phase transition in the Milky Way’s nuclear wind
Noon, K. A., Krumholz, M. R., Teodoro, E. M. D., McClure‐Griffiths, N. M., Lockman, F. J., & Armillotta, L. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1890 · Cited by 19
Systematic effects in the extraction of the `WMAP haze'
Mertsch, P., & Sarkar, S. (2010) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2010/10/019 · Cited by 19
Верходанов, О. В. (2016) · Physics-Uspekhi · doi:10.3367/ufne.0186.201601b.0003 · Cited by 19
Yang, L.-L., & Razzaque, S. (2018) · Physical Review D · doi:10.1103/physrevd.99.083007 · Cited by 35
A magnetized Galactic halo from inner Galaxy outflows
Zhang, H.-S., Ponti, G., Carretti, E., Liu, R.-Y., Morris, M., Haverkorn, M., Locatelli, N., Zheng, X., Aharonian, F., Zhang, H.-M., et al. (2024) · Nature Astronomy · doi:10.1038/s41550-024-02362-0 · Cited by 11
“It is worth noting that the origin of the Fermi bubbles and their potential low-latitude radio counterparts (the so-called radio haze) 18,19 can either be the outflows from the star formation activity of the Central Molecular Zone 20,21 or the past activity of the central supermassive black hole…”
Cosmic microwave background constraints on light dark matter candidates
Evoli, C., Pandolfi, S., & Ferrara, A. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt849 · Cited by 18
“…detection of gamma-rays from the Galactic Centre, the synchrotron emission from the Milky Way radio filaments and the diffuse synchrotron emission from the inner galaxy (the so-called “WMAP Haze”1 (Finkbeiner 2004; Hooper, Finkbeiner & Dobler 2007; Hooper & Linden 2011a,b; Dobler et al. 2010).”
BackgroundA latitude-dependent analysis of the leptonic hypothesis for the Fermi Bubbles
Narayanan, S., & Slatyer, T. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx577 · Cited by 16
“As discussed previously by e.g. Dobler et al. (2010); Su, Slatyer & Finkbeiner (2010); Dobler (2012a); Ackermann et al. (2014), the consistency in the required power-law slopes suggests that the WMAP Haze and the Fermi Bubbles spectrum can be described by the same distribution of high energy…”
BackgroundSelf-citationConstraining Decaying Dark Matter with Fermi LAT Gamma-raysPreprint
Zhang, L., Weniger, C., Maccione, L., Redondo, J., & Günter Sigl, A. (2009) · Cited by 18
Lallement, R. (2022) · Comptes Rendus Physique · doi:10.5802/crphys.97 · Cited by 17
Multimessenger constraints on dark matter annihilation into electron–positron pairs
Wechakama, M., & Ascasíbar, Y. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt2488 · Cited by 17
“The Fermi gamma-ray maps were computed by Dobler et al. (2010) from all ‘Class 3’ (diffuse) photon events in the first-year data release.”
MethodCholis, I., & Goodenough, L. (2016) · Cited by 17
Self-citationWavelet-based techniques for the gamma-ray sky
McDermott, S. D., Fox, P. J., Cholis, I., & Lee, S. K. (2016) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2016/07/045 · Cited by 16
“As in [16{18], we choose to mask the Galactic disk because the low-latitude uncertainties are substantially bigger than the high-latitude uncertainties, and the KS test (which includes no spatial information) is unnecessarily hampered in (cid:12)nding high-latitude emission if all disk-associated…”
Self-citationOka, T., & Geballe, T. R. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abb1b5 · Cited by 16
“This model can be considered as anticipating the discovery of the bipolar γ-ray Fermi Bubbles (Dobler et al. 2010; Su, Slatyer, & Finkbeiner 2010).”
MethodВерходанов, О. В. (2016) · Uspekhi Fizicheskih Nauk · doi:10.3367/ufnr.0186.201601b.0003 · Cited by 16
Discovery of High-velocity Hα Emission in the Direction of the Fermi Bubble
Krishnarao, D., Benjamin, R. A., & Haffner, L. M. (2020) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aba8f0 · Cited by 15
Search for high-energyγ-ray emission from galaxies of the Local Group withFermi/LAT
Lenain, J.-P., & Walter, R. (2011) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201117523 · Cited by 15
Dark Matter inB–Lsupersymmetric Standard Model with inverse seesaw
Abdallah, W., & Khalil, S. (2017) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2017/04/016 · Cited by 15
Fermi bubbles from stochastic acceleration of electrons in a Galactic outflow
Mertsch, P., & Petrosian, V. (2019) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201833999 · Cited by 15
“The search for a counterpart of the microwave haze in gammarays was in fact what motivated the first study that lead to the discovery of the Fermi bubbles (Dobler et al. 2010).”
BackgroundSources of GeV Photons and the Fermi Results
Dermer, C. (2012) · Saas-Fee Advanced Course · doi:10.1007/978-3-642-36134-0_3 · Cited by 17
Ursino, E., Galeazzi, M., & Liu, W.-H. (2015) · The Astrophysical Journal · doi:10.3847/0004-637x/816/1/33 · Cited by 7
“The Fermi Bubbles (Su et al. 2010; Dobler et al. 2010; Ackermann et al. 2014) are large scale (order of some kpc) γ-ray features broadly overlapping Loop I.”
BackgroundTotani, T. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/11/080 · Cited by 14
“Another possible reason is that halo-scale (up to ∼ 50 deg from the GC) diffuse radiation structures, such as the Fermi bubbles [37–39], have been found.”
ANALYSIS OF WMAP 7 YEAR TEMPERATURE DATA: ASTROPHYSICS OF THE GALACTIC HAZE
Pietrobon, D., Górski, K., Bartlett, J., Banday, A., Dobler, G., Colombo, L., Pagano, L., Rocha, G., Saha, R., Jewell, J., et al. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/755/1/69 · Cited by 12
“…with the release of gammaray data from the Fermi Gamma-Ray Space Telescope in 2009, a corresponding feature at high energies was discovered (Dobler et al. 2010), likely generated by the haze electron inverse Compton (IC) scattering starlight, infrared, and CMB photons up to Fermi energies.”
BackgroundMethodSelf-citationON THE ORIGIN OF THE CENTRAL 1″ HOLE IN THE STELLAR DISK OF SGR A* AND THE FERMI GAMMA-RAY BUBBLES
Wardle, M., & Yusef-Zadeh, F. (2014) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/787/1/l14 · Cited by 11
“Two bubbles of γ-ray emission with sharp edges extend symmetrically away from the Galactic plane up to Galactic latitudes b∼ ±500 (Dobler et al. 2010; Su et al. 2010).”
BackgroundKo, C., Breitschwerdt, D., Chernyshov, D. O., Cheng, H., Dai, L., & Dogiel, V. A. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abbda4 · Cited by 15
GALACTIC DIFFUSE GAMMA RAYS—RECALCULATION BASED ON NEW MEASUREMENTS OF THE COSMIC ELECTRON SPECTRUM
Zhang, J., Yuan, Q., & Bi, X.-J. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/720/1/9 · Cited by 14
Testing the dark matter annihilation model for the Wilkinson Microwave Anisotropy Probe haze
McQuinn, M., & Zaldarriaga, M. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18658.x · Cited by 13
Stochastic Acceleration of Cosmic Rays in the Central Molecular Zone of the Galaxy
Amano, T., Torii, K., Hayakawa, T., & Fukui, Y. (2011) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/63.6.l63 · Cited by 13
“Such a scenario seems natural in view of recently found Fermi bubbles (Su et al., 2010; Dobler et al., 2010), while so far there is no direct evidence for the wind.”
BackgroundDiffuse Galactic Gamma Rays at intermediate and high latitudes. I. Constraints on the ISM properties
Cholis, I., Tavakoli, M., Evoli, C., Maccione, L., & Ullio, P. (2011) · DESY (CERN, DESY, Fermilab, IHEP, and SLAC) · Cited by 13
Self-citationFermi bubbles: the collimated outburst needed to explain forward-shock edges
Mondal, S., Keshet, U., Sarkar, K. C., & Gurwich, I. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1084 · Cited by 13
Unveiling the Origin of the Fermi Bubbles with MeV Photon Telescopes
Negro, M., Fleischhack, H., Zoglauer, A. C., Digel, S. W., & Ajello, M. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac5326 · Cited by 13
Fermi bubbles: high-latitude X-ray supersonic shell
Keshet, U., & Gurwich, I. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1533 · Cited by 13
“This scenario was revived by the discovery (Dobler et al. 2010; Su et al. 2010, henceforth S10) of two large γ-ray, so called Fermi, bubbles (FBs), symmetrically rising far from the Milky-Way plane yet morphologically connected, at least approximately and in projection, to the intermediate scale…”
BackgroundDiverse metallicities of Fermi bubble clouds indicate dual origins in the disk and halo
Ashley, T., Fox, A. J., Cashman, F. H., Lockman, F. J., Bordoloi, R., Jenkins, E. B., Wakker, B. P., & Karim, T. (2022) · Nature Astronomy · doi:10.1038/s41550-022-01720-0 · Cited by 12
The Interaction of the Active Nucleus with the Host Galaxy Interstellar Medium
Fabbiano, G., & Elvis, M. (2023) · Springer eBooks · doi:10.1007/978-981-16-4544-0_111-1 · Cited by 17
Cook, R. H. W., Seymour, N., Spekkens, K., Hurley-Walker, N., Hancock, P. J., Bell, M. E., Callingham, J. R., For, B., Franzen, T. M. O., Gaensler, B. M., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa726 · Cited by 12
“Examples of such objects include: the Galactic centre (e.g., Abazajian & Harding 2012; Abdo et al. 2010a, Ackermann et al. 2012a; Dobler et al. 2010), diffuse Galactic and extragalactic backgrounds (e.g., Abdo et al. 2010b; Papucci & Strumia 2010; Baxter &Dodelson 2011); as well as galaxy clusters…”
BackgroundFermi bubbles from stochastic acceleration of electrons in a Galactic outflow
Mertsch, P., & Petrosian, V. (2019) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201833999/pdf · Cited by 12
Galactic halo bubble magnetic fields and UHECR deflections
Shaw, V., van Vliet, A., & Taylor, A. M. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2778 · Cited by 12
On the Origin of the Central 1” Hole in the Stellar Disk of Sgr A* and the Fermi Gamma-Ray BubblesPreprint
Wardle, M., & Yusef-Zadeh, F. (2014) · Cited by 12
Hadronic Models of the Fermi Bubbles: Future Perspectives
Razzaque, S., & Yang, L. (2018) · Galaxies · doi:10.3390/galaxies6020047 · Cited by 11
Caron, S., Eckner, C., Hendriks, L., Jóhannesson, G., de Austri, R. R., & Zaharijaš, G. (2023) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2023/06/013 · Cited by 14
“The base of the Fermi bubbles (FB), a large structure centered at the GC [13, 14], is also expected to contribute to the measured emission, though the bubbles are challenging to detect close to the Galactic plane.”
BackgroundMorphological analysis of the polarized synchrotron emission with WMAP and Planck
Martire, F. A., Banday, A. J., Martínez-González, E., & Barreiro, R. B. (2023) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2023/04/049 · Cited by 11
“Because of their location, there are models which link these structures with the Fermi Bubbles (FB) detected in Fermi data at energies ∼10–500 GeV [47, 48].”
BackgroundThe spectral index of polarized diffuse Galactic emission between 30 and 44 GHz
Jew, L., & Grumitt, R. D. P. (2019) · Monthly notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1233 · Cited by 9
Revealing Gas Inflows Toward the Galactic Central Molecular Zone
Su, Y., Zhang, S., Sun, Y., Yang, J., YAN, Q.-Z., Zhang, S., Chen, Z., Chen, X., Zhou, X., & Yuan, L. (2024) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ad656d · Cited by 12
Metal Enrichment in the Fermi Bubbles as a Probe of Their Origin
Inoue, Y., Nakashima, S., Tahara, M., Kataoka, J., Totani, T., Fujita, Y., & Sofue, Y. (2015) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psv032 · Cited by 10
“The Fermi bubbles are gigantic gamma-ray structures extending∼ 50◦ north and south of the Galactic center (GC) with a longitudinal with∼ 40◦ (Dobler et al., 2010; Su et al., 2010; Ackermann et al., 2014).”
BackgroundGaisser, T., & Stanev, T. (2012) · Astroparticle Physics · doi:10.1016/j.astropartphys.2012.08.004 · Cited by 11
IceCube Constraints on the Fermi Bubbles
Sherf, N., Keshet, U., & Gurwich, I. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa894f · Cited by 10
“A pair of highly extended, double-lobed γ-ray bubbles was identified (Dobler et al. 2010; Su et al. 2010, henceforth S10) using the Fermi-LAT data.”
MethodSchulreich, M. M., & Breitschwerdt, D. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2940 · Cited by 10
MiXDM: Cosmic Ray Signals from Multiple States of Dark MatterPreprint
Cholis, I., & Weiner, N. (2009) · arXiv (Cornell University) · doi:10.48550/arxiv.0911.4954 · Cited by 10
“BFχ 2 = 120 B-field I, Sommerfeld Enh. Fermi Haze Template (|l| ≤ 15, -30 ≤ b ≤ -10) 1:1 2:1 3:1 4:1 Figure 5: A comparison of the residual Fermi Haze data |l| < 10◦ and 10◦ < |b| < 30◦ from [81], versus DM ICS contributions for uniform boost and an Einasto profile (left) and with a v−1 scaling assuming vdisp…”
MethodInfluentialSelf-citationMAXI/SSC all-sky maps from 0.7 keV to 4 keV
Nakahira, S., Tsunemi, H., Tomida, H., Nakashima, S., Kataoka, R., & Makishima, K. (2020) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psz139 · Cited by 9
“Namely, a giant Galactic gamma-ray structure was discovered by the Fermi Gamma-Ray Space Telescope, in the energy range of 1-10 GeV (Dobler et al. 2010).”
BackgroundCholis, I. (2012) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.88.063524 · Cited by 6
Self-citationEmission from hadronic and leptonic processes in galactic jet-driven bubbles
Owen, E. R., & Yang, H.-Y. K. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2289 · Cited by 9
Can a satellite galaxy merger explain the active past of the Galactic Centre?
Lang, M., Holley‐Bockelmann, K., Bogdanović, T., Amaro‐Seoane, P., Sesana, A., & Sinha, M. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sts638 · Cited by 9
“The gamma-ray bubbles exhibit several striking properties: they are perpendicular and symmetric with respect to the plane of the Galaxy, have nearly uniform gamma-ray brightness across the bubbles and well-defined sharp edges (Dobler et al. 2010; Su et al. 2010).”
BackgroundMou, G.-B., Sun, D., & Xie, F. (2018) · Astrophysical Journal · doi:10.3847/2041-8213/aaf421 · Cited by 8
“Two giant gamma-ray bubbles located symmetrically above and below the Galactic plane are revealed by the Fermi Gamma-ray Space Telescope (Dobler et al. 2010; Su et al. 2010; Ackermann et al. 2014).”
MethodPhysical laboratory at the center of the Galaxy
Dokuchaev, V. I., & Eroshenko, Y. N. (2015) · Uspekhi Fizicheskih Nauk · doi:10.3367/ufnr.0185.201508c.0829 · Cited by 11
The Important Role of Cosmic-Ray Re-Acceleration
Cardillo, M. (2019) · Galaxies · doi:10.3390/galaxies7020049 · Cited by 8
“Stochastic re-acceleration could even explain γ-ray emission from Fermi-Bubbles [52,53] as shown in the work of [35].”
Bentley, R. O., Do, T., Kerzendorf, W., Chu, D. S., Chen, Z., Konopacky, Q., & Ghez, A. M. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac3910 · Cited by 8
Omar, A. (2022) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slac081 · Cited by 8
Our supermassive black hole rivaled the Sun in the ancient X-ray sky
Amaro‐Seoane, P., & Chen, X. (2019) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2019/12/056 · Cited by 10
Metal Enrichment in the Fermi Bubbles as a Probe of their Origin
Inoue, Y., Nakashima, S., Tahara, M., Kataoka, J., Totani, T., Fujita, Y., Sofue, Y., 中島, 真., 田原, 将., 片岡, 淳., et al. (2015) · JAXA Repository (JAXA) · Cited by 8
Feasibility of Correlated Extensive Air Shower Detection with a Distributed Cosmic-Ray Network
Albin, E. K., & Whiteson, D. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acc52d · Cited by 7
Fermi bubbles as a source of cosmic rays above 1015 eV
Chernyshov, D., Cheng, K.-S., Dogiel, V., & Ko, C.-M. (2014) · Nuclear Physics B - Proceedings Supplements · doi:10.1016/j.nuclphysbps.2014.10.021 · Cited by 4
Koljonen, K. I. I., Lindseth, S. S., Linares, M., Harding, A. K., & Turchetta, M. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae498 · Cited by 6
Cosmic Censorship in Sgr A* and M87*: Observationally Excluding Naked Singularities
Broderick, A. E., & Salehi, K. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad90aa · Cited by 14
Quark nugget dark matter: Comparison with radio observations of nearby galaxies
Lawson, K., & ZHITNITSKY, A. R. (2016) · Physics Letters B · doi:10.1016/j.physletb.2016.04.024 · Cited by 6
Emission from hadronic and leptonic processes in galactic jet-driven bubbles
Owen, E. R., & Yang, H.-Y. K. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac119 · Cited by 10
Testing the dark matter origin of the WMAP-Planck haze with radio observations of spiral galaxies
Carlson, E., Hooper, D., Linden, T., & Profumo, S. (2013) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2013/07/026
“Recent observations indicate that the observed morphology of the microwave excess haze exhibits a strong correlation with a diffuse feature discovered at GeV energies by the Fermi Large Area Telescope, known as the Fermi bubbles [45] (previously known as “Fermi haze” [46], see also [47]).”
BackgroundCOSMIC RAY ACCELERATORS IN THE LARGE MAGELLANIC CLOUD
Butt, Y. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/725/1/1 · Cited by 6
Metadata
- Authors
- Dobler, G., Finkbeiner, D. P., Cholis, I., Slatyer, T., & Weiner, N.
- Affiliations
- Harvard University (US)
- New York University (US)
- Corresponding author
- Dobler, Gregory
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2010-06-18
- Volume
- 717
- Issue
- 2
- Pages
- 825-842
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W1980231566
- Cited by
- 285
- References
- 34
- Citations by year
- 2026: 2 · 2025: 4 · 2024: 9 · 2023: 13 · 2022: 17 · 2021: 8 · 2020: 15 · 2019: 12 · 2018: 15 · 2017: 19 · 2016: 23 · 2015: 28 · 2014: 19 · 2013: 28 · 2012: 32
- FWCI
- 17.77
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- Digital Access to Scholarship at Harvard (DASH) (Harvard University) (submittedVersion, cc-by)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Astrophysics and Cosmic Phenomena
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Gamma-ray bursts and supernovae
- Keywords
- Fermi Gamma-ray Space Telescope, inverse Compton scattering, Galactic Center gamma-ray excess, synchrotron radiation, electron energy spectrum, bremsstrahlung, diffuse gamma-ray emission, inner Galaxy
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