THE SPECTRUM AND MORPHOLOGY OF THE FERMI BUBBLES
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The Fermi bubbles are two large structures in the gamma-ray sky extending to 55° above and below the Galactic center. We analyze 50 months of Fermi Large Area Telescope data between 100 MeV and 500 GeV above 10° in Galactic latitude to derive the spectrum and morphology of the Fermi bubbles. We thoroughly explore the systematic uncertainties that arise when modeling the Galactic diffuse emission through two separate approaches. The gamma-ray spectrum is well described by either a log parabola or a power law with an exponential cutoff. We exclude a simple power law with more than 7σ significance. The power law with an exponential cutoff has an index of 1.9 ± 0.2 and a cutoff energy of 110 ± 50 GeV. We find that the gamma-ray luminosity of the bubbles is erg s −1 . We confirm a significant enhancement of gamma-ray emission in the southeastern part of the bubbles, but we do not find significant evidence for a jet. No significant variation of the spectrum across the bubbles is detected. The width of the boundary of the bubbles is estimated to be deg. Both inverse Compton (IC) models and hadronic models including IC emission from secondary leptons fit the gamma-ray data well. In the IC scenario, synchrotron emission from the same population of electrons can also explain the WMAP and Planck microwave haze with a magnetic field between 5 and 20 μG.
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The steepening of the γ-ray spectrum could simply be due to the lack of cosmic-ray electron acceleration at energies ≳TeV.
“A general fit assuming a CRe population containing a simple power law and an exponential cutoff, i.e. N ∝ Γ -2 . 2 exp( -Γ / 2 . 5 × 10 6 ), has also been shown to fit well with the FB spectra (Su et al. 2010; Ackermann et al. 2014) indicating that the steepening of the γ -ray spectrum could simply be due to the lack of CRe acceleration at Ee ≳ TeV.”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Ackermann et al. 2014
Section 7.1 (p. 44) reports that an electron spectrum with an exponential cutoff at 1.25 TeV fits the Fermi-bubble γ-ray spectrum. But the Summary and conclusions (p. 53) says the cutoff can be explained by electron cooling from inverse-Compton and synchrotron losses; it does not attribute the cutoff to a lack of electron acceleration above TeV energies. (LLM, conf=0.86)
Experimental — accuracy not yet measuredComplete integration in the 0.1-500 GeV range produces a γ-ray luminosity of ≃4×10^37 erg s^-1, for an assumed distance of 9.4 kpc to the center of the FBs and a total size of 0.66 sr.
“Complete integration in the 0 . 1 -500 GeV range produces a γ -ray luminosity of ≃ 4 × 10 37 erg s -1 , for an assumed distance of 9 . 4 kpc to the center of the FBs and a total size of 0 . 66 sr (Su et al. 2010; Ackermann et al. 2014).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Ackermann et al. 2014
The outer edge of the NPS falls precisely on the outer edge of the Haslam 408 MHz radio map, 28.4 GHz map, and the γ-ray residual map of the soft component, indicating a common origin.
“The outer edge of the NPS also falls precisely on the outer edge of the Haslam 408 MHz radio map (Haslam et al. 1982), 28 . 4 GHz map (Planck Collaboration et al. 2016), and the γ -ray residual map of the soft component (figure 2; Ackermann et al. 2014) indicating a common origin.”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Ackermann et al. 2014
The origin of the diffuse γ-ray emission in our Galaxy can be attributed to three main processes: Hadronic, Bremsstrahlung, and Inverse Compton (IC).
“The origin of the diffuse γ -ray emission in our Galaxy can be attributed to three main processes Hadronic , Bremsstrahlung , and Inverse Compton (IC) (Fichtel et al. 1978; Su et al. 2010; Ackermann et al. 2014).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Ackermann et al. 2014
The typical magnetic field in the haze is B ∼ 8 μG.
“Further analysis of the microwave spectrum showed that the typical magnetic field in the haze is, B ∼ 8 µ G (Su et al. 2010; Dobler 2012; Ackermann et al. 2014; Narayanan & Slatyer 2017).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Ackermann et al. 2014
A general fit assuming a cosmic-ray electron population containing a simple power law and an exponential cutoff, N∝Γ^-2.2 exp(-Γ/2.5×10^6), has been shown to fit well with the Fermi bubble spectra.
“A general fit assuming a CRe population containing a simple power law and an exponential cutoff, i.e. N ∝ Γ -2 . 2 exp( -Γ / 2 . 5 × 10 6 ), has also been shown to fit well with the FB spectra (Su et al. 2010; Ackermann et al. 2014) indicating that the steepening of the γ -ray spectrum could simply be due to the lack of CRe acceleration at Ee ≳ TeV.”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Ackermann et al. 2014
Although the p-p channel can successfully explain the γ-ray spectrum from the Fermi bubbles, the synchrotron emission from secondary leptonic particles fails to explain the spectrum or intensity of the microwave haze emission.
“Although the p -p channel can successfully explain the γ -ray spectrum from the FBs, the synchrotron emission from the secondary leptonic particles fails to explain the spectrum or the intensity of the microwave haze emission (Ackermann et al. 2014; Crocker et al. 2015; Cheng et al. 2015a).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Ackermann et al. 2014
One big advantage of the leptonic origin of the γ-ray is that the same cosmic-ray electron population can also explain the spectrum and intensity of the microwave haze.
“One big advantage of the leptonic origin of the γ -ray is that the same CRe population can also explain the spectrum and intensity of the microwave haze (Su et al. 2010; Planck Collaboration et al. 2013; Ackermann et al. 2014).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Ackermann et al. 2014
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The Galactic center chimneys: the base of the multiphase outflow of the Milky Way
Ponti, G., Morris, M., Churazov, E., Heywood, I., & Fender, R. P. (2021) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/202039636/pdf · Cited by 40 · see citing works
Ade, P. A. R., Aghanim, N., Aniano, G., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., et al. (2015) · Maynooth University ePrints and eTheses Archive (Maynooth University) · doi:10.1051/0004-6361/201424955 · Cited by 36 · see citing works
Self-citationThe Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way
Sarkar, K. C. (2024) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-024-00152-1 · Cited by 34 · see citing works
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 · see citing works
- Authors
- Ackermann, M., Albert, A., Atwood, W. B., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bellazzini, R., Bissaldi, E., Blandford, R. D., Bloom, E. D., Bottacini, E., Brandt, T. J., Bregeon, J., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Cecchi, C., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Claus, R., Cohen-Tanugi, J., Conrad, J., Cutini, S., D'Ammando, F., de Angelis, A., de Palma, F., Dermer, C. D., Digel, S. W., Venere, L. D., do Couto e Silva, E., Drell, P. S., Favuzzi, C., Ferrara, E. C., Focke, W. B., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Germani, S., Giglietto, N., Giordano, F., Giroletti, M., Godfrey, G., Gomez-Vargas, G. A., Grenier, I. A., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hou, X., Jogler, T., Jóhannesson, G., Johnson, A. S., Johnson, W. N., Kamae, T., Kataoka, J., Knödlseder, J., Kocevski, D., Kuss, M., Larsson, S., Latronico, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Malyshev, D., Manfreda, A., Massaro, F., Mayer, M., Mazziotta, M. N., McEnery, J. E., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nemmen, R., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Perkins, J. S., Pesce-Rollins, M., Petrosian, V., Piron, F., Pivato, G., Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Sánchez-Conde, M., Schaal, M., Schulz, A., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Stawarz, Ł., Strong, A. W., Suson, D. J., Tahara, M., Takahashi, H., Thayer, J. B., Tibaldo, L., Tinivella, M., Torres, D. F., Tosti, G., Troja, E., Uchiyama, Y., Vianello, G., Werner, M., Winer, B. L., Wood, K. S., Wood, M., & Zaharijas, G.
- Affiliations
- Deutsches Elektronen-Synchrotron DESY (DE)
- SLAC National Accelerator Laboratory (US)
- University of California, Santa Cruz (US)
- Istituto Nazionale di Fisica Nucleare, Sezione di Pisa (IT)
- Centre National de la Recherche Scientifique (FR)
- University of Trieste (IT)
- University of Padua (IT)
- Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (IT)
- Goddard Space Flight Center (US)
- Istituto Nazionale di Fisica Nucleare, Sezione di Bari (IT)
- Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano (IT)
- Agenzia Spaziale Italiana (IT)
- George Mason University (US)
- Astronomical Observatory of Rome (IT)
- Royal Swedish Academy of Sciences (SE)
- Istituto di Radioastronomia di Bologna (IT)
- United States Naval Research Laboratory (US)
- University of Bari Aldo Moro (IT)
- Hiroshima University (JP)
- University of Perugia (IT)
- Universität Innsbruck (AT)
- University of Iceland (IS)
- Waseda University (JP)
- Stockholm University (SE)
- Istituto Nazionale di Fisica Nucleare, Sezione di Torino (IT)
- Yale University (US)
- Mahidol University (TH)
- University of California, Irvine (US)
- University of Denver (US)
- University of Johannesburg (ZA)
- National Academy of Sciences (US)
- Jagiellonian University (PL)
- Max Planck Institute for Extraterrestrial Physics (DE)
- Purdue University Northwest (US)
- Institució Catalana de Recerca i Estudis Avançats (ES)
- The Ohio State University (US)
- Corresponding author
- Malyshev, D.
- ORCID
- Ackermann, M.
- Albert, A.
- Baldini, L.
- Ballet, J.
- Bastieri, D.
- Bellazzini, R.
- Bissaldi, E.
- Blandford, R. D.
- Bottacini, E.
- Brandt, T. J.
- Bregeon, J.
- Bruel, P.
- Buehler, R.
- Buson, S.
- Cameron, R. A.
- Caraveo, P. A.
- Cavazzuti, E.
- Charles, E.
- Chekhtman, A.
- Chiang, J.
- Chiaro, G.
- Ciprini, S.
- Cohen-Tanugi, J.
- Cutini, S.
- D'Ammando, F.
- Dermer, C. D.
- Digel, S. W.
- Venere, L. Di
- Ferrara, E. C.
- Franckowiak, A.
- Fukazawa, Y.
- Funk, S.
- Fusco, P.
- Gargano, F.
- Gasparrini, D.
- Germani, S.
- Giglietto, N.
- Giordano, F.
- Giroletti, M.
- Grenier, I. A.
- Guiriec, S.
- Hadasch, D.
- Harding, A. K.
- Hays, E.
- Hewitt, J. W.
- Hou, X.
- Jogler, T.
- Jóhannesson, G.
- Johnson, A. S.
- Kataoka, J.
- Kocevski, D.
- Kuss, M.
- Larsson, S.
- Latronico, L.
- Longo, F.
- Loparco, F.
- Lovellette, M. N.
- Lubrano, P.
- Malyshev, D.
- Manfreda, A.
- Massaro, F.
- Mayer, M.
- Mazziotta, M. N.
- Michelson, P. F.
- Mitthumsiri, W.
- Mizuno, T.
- Monzani, M. E.
- Moskalenko, I. V.
- Murgia, S.
- Nemmen, R.
- Nuss, E.
- Omodei, N.
- Orienti, M.
- Orlando, E.
- Ormes, J. F.
- Paneque, D.
- Perkins, J. S.
- Pesce-Rollins, M.
- Petrosian, V.
- Piron, F.
- Pivato, G.
- Rainò, S.
- Rando, R.
- Razzano, M.
- Razzaque, S.
- Reimer, A.
- Reimer, O.
- Sánchez-Conde, M.
- Siskind, E. J.
- Spandre, G.
- Spinelli, P.
- Stawarz, Łukasz
- Strong, A. W.
- Suson, D. J.
- Takahashi, H.
- Thayer, J. B.
- Tibaldo, L.
- Torres, D. F.
- Tosti, G.
- Troja, E.
- Uchiyama, Y.
- Vianello, G.
- Werner, M.
- Winer, B. L.
- Wood, K. S.
- Wood, M.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2014-09-05
- Volume
- 793
- Issue
- 1
- Pages
- 64
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2165063682
- Cited by
- 328
- References
- 55
- Citations by year
- 2026: 10 · 2025: 11 · 2024: 21 · 2023: 21 · 2022: 23 · 2021: 26 · 2020: 21 · 2019: 25 · 2018: 36 · 2017: 33 · 2016: 48 · 2015: 50 · 2014: 2 · 2013: 1
- FWCI
- 19.55
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Licence
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- Desy publication database (The Deutsches Elektronen-Synchrotron) (submittedVersion, other-oa)
- Institutional Research Information System University of Turin (University of Turin) (submittedVersion)
- OSTI OAI (U.S. Department of Energy Office of Scientific and Technical Information) (submittedVersion)
- Jagiellonian University Repository (Jagiellonian University) (submittedVersion, cc-by-nc-nd)
- HAL (submittedVersion)
- CINECA IRIS Institutial research information system (University of Pisa) (submittedVersion, cc-by-nc-nd)
- ArTS Archivio della ricerca di Trieste (University of Trieste https://www.units.it/) (submittedVersion)
- Archivio istituzionale della ricerca (Alma Mater Studiorum Università di Bologna) (submittedVersion)
- UCL Discovery (University College London) (submittedVersion)
- Max Planck Digital Library (submittedVersion)
- Institutional Repositories DataBase (IRDB) (submittedVersion)
- AIRUS (submittedVersion)
- Oskar-Bordeaux (Universite de Bordeaux) (submittedVersion)
- MPG.PuRe (Max Planck Society) (submittedVersion)
- JAXA Repository (JAXA) (submittedVersion, cc-by-nc-nd)
- CINECA IRIS Institutional Research Information System (University of Bari Aldo Moro) (submittedVersion)
- Padua Research Archive (University of Padova) (submittedVersion)
- arXiv (Cornell University)
- DESY Publication Database (PUBDB) (Deutsches Elektronen-Synchrotron)
- 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 › Astrophysical Phenomena and Observations
- Keywords
- Fermi bubbles, gamma-ray spectra, gamma-ray morphology, Galactic diffuse emission, inverse Compton emission, hadronic interaction models, synchrotron radiation, cosmic ray acceleration, Galactic Center, gamma-ray luminosity, magnetic field
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