Survey of the Galactic Plane with the Cherenkov Telescope Array

Remy, Quentin; Tibaldo, L.; Acero, Fabio; Fiori, Michele; Knödlseder, Jürgen; Olmi, Barbara; Sharma, Priyanka

doi:10.22323/1.395.0886

Cited by 16 publications

(24 citation statements)

References 106 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This may indicate either the mismodeling of 3HWC J1928+178 or the lack of a large-scale galactic diffuse emission component in the model. We checked the expected flux of the galactic diffuse emission underlying the three sources J1928, J1930, and J1932 by using four different models: the latest Fermi model for Pass 8 and source class events (Abdollahi et al 2020), the diffuse emission model developed to simulate the Galactic plane survey with the future Cherenkov Telescope Array (CTA) (Remy et al 2021), an updated version of this model (private communication with Q. Remy), and a model of the galactic diffuse emission up to 100 TeV developed by De la Torre Luque et al (2022). On average, the contribution from J1928-EXT to these sources is more than twice the average flux that is expected from the galactic diffuse emission.…”

Section: Discussionmentioning

confidence: 99%

Detailed Analysis of the TeV γ-Ray Sources 3HWC J1928+178, 3HWC J1930+188, and the New Source HAWC J1932+192

Albert

Aguilera

Álvarez

et al. 2023

ApJ

View full text Add to dashboard Cite

The latest High Altitude Water Cherenkov (HAWC) point-like source catalog up to 56 TeV reported the detection of two sources in the region of the Galactic plane at galactic longitude 52° < ℓ < 55°, 3HWC J1930+188 and 3HWC J1928+178. The first one is associated with a known TeV source, the supernova remnant SNR G054.1+00.3. It was discovered by one of the currently operating Imaging Atmospheric Cherenkov Telescope (IACT), the Very Energetic Radiation Imaging Telescope Array System (VERITAS), detected by the High Energy Stereoscopic System (H.E.S.S), and identified as a composite SNR. However, the source 3HWC J1928+178, discovered by HAWC and coincident with the pulsar PSR J1928+1746, was not detected by any IACT despite their long exposure on the region, until a recent new analysis of H.E.S.S. data was able to confirm it. Moreover, no X-ray counterpart has been detected from this pulsar. We present a multicomponent fit of this region using the latest HAWC data. This reveals an additional new source, HAWC J1932+192, which is potentially associated with the pulsar PSR J1932+1916, whose γ-ray emission could come from the acceleration of particles in its pulsar wind nebula. In the case of 3HWC J1928+178, several possible explanations are explored, in an attempt to unveil the origins of the very-high-energy γ-ray emission.

show abstract

Section: Discussionmentioning

confidence: 99%

Detailed Analysis of the TeV γ-Ray Sources 3HWC J1928+178, 3HWC J1930+188, and the New Source HAWC J1932+192

Albert

Aguilera

Álvarez

et al. 2023

ApJ

View full text Add to dashboard Cite

show abstract

“…of them are actually PWNe with no direct association with a known pulsar. As we already said, thanks to their longer lifetime as gamma-ray emitters, middle aged PWNe will likely dominate the very high energy sky, possibly representing up to 60% of the Galactic sources, and a huge number of new detection ( 200) may be expected with the upcoming Cherenkov Telescope Array, thanks to its unprecedented angular and energy resolution (Remy et al 2022; Fiori et al 2022). A very challenging problem will be that of the source confusion in the crowded Galactic plane, that will reduce the number of identified sources with respect to theoretical estimate (Mestre et al 2022).…”

Section: Where We Are and Where We Gomentioning

confidence: 98%

“…Faucher-Giguere & Kaspi 2006), so that one can safely consider the PSR to be stationary at this stage. During this phase, the evolution of the PWN is independent from that of the SNR shell, since no interaction has been established yet between the two (Reynolds & Chevalier 1984). Based on the results by Jun (1998), showing that the PWN collects material in a thin-shell at its boundary during its initial expansion (t τ 0 ), a simplified description of the PWN evolution can be obtained using the following formulas:…”

Section: Free Expansionmentioning

confidence: 99%

“…If compared with water Cherenkov detectors, as LHAASO or Tibet As- , they will operate in a reduced energy range but with a much better sensitivity and resolution. As a consequence, the number of PWNe detected at gamma rays is expected to increase significantly (Fiori et al 2022; Remy et al 2022), posing the problem of the identification of a very large number of new PWNe, mostly in their middle-age stage.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The Dawes Review 11: From young to old: The evolutionary path of Pulsar Wind Nebulae

Olmi

Bucciantini

2023

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

Pulsar wind nebulae are fascinating systems, and archetypal sources for high-energy astrophysics in general. Due to their vicinity, brightness, to the fact that they shine at multi-wavelengths, and especially to their long-living emission at gamma-rays, modelling their properties is particularly important for the correct interpretation of the visible Galaxy. A complication in this respect is the variety of properties and morphologies they show at different ages. Here we discuss the differences among the evolutionary phases of pulsar wind nebulae, how they have been modeled in the past and what progresses have been recently made. We approach the discussion from a phenomenological, theoretical (especially numerical) and observational point of view, with particular attention to the most recent results and open questions about the physics of such intriguing sources.

show abstract

“…There is detailed online documentation of the package 15 with a user guide, API reference and many detailed tutorials using different kind of data ranging from HESS, MAGIC, HAWC, simulated CTA, GeV energy Fermi-LAT data and even combinations thereof. Gammapy is designed both for interactive use in Jupyter notebooks 16 but also large scale offline analyses such as the upcoming CTA Galactic Plane Survey [654].…”

Section: Snowmass2021 Cf07 Gamma-ray Experimentsmentioning

confidence: 99%

The Future of Gamma-Ray Experiments in the MeV-EeV Range

Engel¹,

Goodman²,

Huentemeyer³

et al. 2022

Preprint

View full text Add to dashboard Cite

Naturally occurring particle accelerators shine brightly throughout the universe, inviting us to discover fundamental laws and hone our theories if we look in their directions with the right detectors. Gamma-rays, the most energetic photons, carry information from the far reaches of extragalactic space with minimal interaction or loss of information. They bring messages about particle acceleration in environments so extreme they cannot be reproduced on earth for a closer look. Gamma-ray astrophysics is so complementary with collider work that particle physicists and astroparticle physicists are often one in the same.Gamma-ray instruments, especially the Fermi Gamma-ray Space Telescope, have been pivotal in major multi-messenger discoveries over the past decade. There is presently a great deal of interest and scientific expertise available to push forward new technologies, to plan and build space-and ground-based gamma-ray facilities, and to build multimessenger networks with gamma rays at their core. It is therefore concerning that before the community comes together for planning exercises again, much of that infrastructure could be lost to a lack of long-term planning for support of gamma-ray astrophysics. Gamma-rays with energies from the MeV to the EeV band are therefore central to multiwavelength and multi-messenger studies to everything from astroparticle physics with compact objects, to dark matter studies with diffuse large scale structure.These science goals and the excitement of new discoveries have generated a wave of new gamma-ray facility proposals and programs. Since the legacy of existing facilities is well covered in many other places, this paper highlights new and proposed gamma-ray technologies and facilities that have each been designed to address specific needs in the measurement of extreme astrophysical sources that probe some of the most pressing questions in fundamental physics for the next decade. The proposed instrumentation would also address the priorities laid out in the recent Decadal Survey of Astronomy and Astrophysics (Astro2020), a complementary study by the astrophysics community that provides opportunities also relevant to Snowmass.

show abstract

Survey of the Galactic Plane with the Cherenkov Telescope Array

Cited by 16 publications

References 106 publications

Detailed Analysis of the TeV γ-Ray Sources 3HWC J1928+178, 3HWC J1930+188, and the New Source HAWC J1932+192

Detailed Analysis of the TeV γ-Ray Sources 3HWC J1928+178, 3HWC J1930+188, and the New Source HAWC J1932+192

The Dawes Review 11: From young to old: The evolutionary path of Pulsar Wind Nebulae

The Future of Gamma-Ray Experiments in the MeV-EeV Range

Contact Info

Product

Resources

About