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Journal articles on the topic 'Galactic Centre Lobe (GCL)'

Author: Grafiati

Published: 6 September 2023

Last updated: 31 July 2025

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1

Sofue, Yoshiaki. "The Galactic Center Lobe." Publications of the Astronomical Society of Japan 37, no. 4 (1985): 697–713. https://doi.org/10.1093/pasj/37.4.697.

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Abstract Radio continuum observations of the central region of our Galaxy have revealed an off-plane, Ω-shaped lobe (the galactic center lobe: GCL) with a diameter 200 pc emerging from the nuclear disk toward the positive galactic latitude. The radio spectrum is flat, indicating either a thermal gas origin or synchrotron radiation due to recently accelerated cosmicray electrons. CO line observations show an association of a high-velocity molecular gas with the lobe ridges. The eastern and western lobe ridges are connected to the “radio arc” and Sgr C in which extremely thin filamentary structu

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2

Anderson, L. D., Matteo Luisi, B. Liu, et al. "The Galactic Center Lobe as an H ii Region." Astrophysical Journal 969, no. 1 (2024): 43. http://dx.doi.org/10.3847/1538-4357/ad4d93.

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Abstract The Galactic center lobe (GCL) is an object ∼1° across that is located north of the Galactic center. In the mid-infrared (MIR) the GCL appears as two 8.0 μm filaments between which there is strong 24 μm and radio continuum emission. Due to its morphology and location in the sky, previous authors have argued that the GCL is located in the Galactic center region, created by outflows from star formation or by activity of the central black hole Sagittarius A*. In an associated paper, low-frequency radio emission indicates that the GCL must instead lie foreground to the Galactic center. If

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3

Hurley-Walker, Natasha, L. D. Anderson, M. Luisi, et al. "Low-frequency Absorption and Radio Recombination Line Features of the Galactic Center Lobe." Astrophysical Journal 969, no. 1 (2024): 42. http://dx.doi.org/10.3847/1538-4357/ad4d92.

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Abstract The Galactic center lobe (GCL) is a ∼1° object located north of the Galactic center. In the mid-infrared, the GCL appears as two 8.0 μm filaments that roughly define an ellipse. There is strong 24 μm and radio continuum emission in the interior of the ellipse. Due to its morphology and location in the sky, previous authors have argued that the GCL is created by outflows from star formation in the central molecular zone or by activity of the central black hole Sgr A*. We present images of the GCL from the GaLactic and Extragalactic All-sky Murchison Widefield Array survey in radio cont

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4

Nagoshi, Halca, Kenta Fujisawa, and Yuzo Kubose. "Radio continuum and radio recombination line observations of the Galactic center lobe." Proceedings of the International Astronomical Union 9, S303 (2013): 129–31. http://dx.doi.org/10.1017/s1743921314000374.

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AbstractRadio continuum (cont) and radio recombination line (RRL) observations with the Yamaguchi 32-m radio telescope toward the lower part of the Galactic center lobe (GCL) in the Galactic center region are presented. While two ridges of the GCL were seen in both continuum and RRL images, the spatial coverage of the ridges of the continuum and RRL is not coincident. We distinguish the continuum emission of the GCL into thermal and non-thermal emission by assuming an electron temperature of the ionized gas of 4370 K, estimated based on the line width (14.1 km s−1). The thermal emission was fo

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5

Rickert, M., F. Yusef-Zadeh, and C. Brogan. "Low frequency (74 MHz) radio continuum observations of the inner 13° × 7° of the Galactic center." Proceedings of the International Astronomical Union 9, S303 (2013): 464–66. http://dx.doi.org/10.1017/s1743921314001161.

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AbstractWe analyze a high resolution (114″ × 60″) 74 MHz image of the Galactic center taken with the Very Large Array (VLA). We have identified several absorption and emission features in this region, and we discuss preliminary results of two Galactic center sources: the Sgr D complex (G1.1–0.1) and the Galactic center lobe (GCL).The 74 MHz image displays the thermal and nonthermal components of Sgr D and we argue the Sgr D supernova remnant (SNR) is consistent with an interaction with a nearby molecular cloud and the location of the Sgr D Hii region on the near side of the Galactic center. Th

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6

Law, Casey. "Evidence for a Mass Outflow from Our Galactic Center." Proceedings of the International Astronomical Union 3, S250 (2007): 407–12. http://dx.doi.org/10.1017/s1743921308020760.

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AbstractWe discuss the nature of the Galactic center lobe (GCL), a degree-tall, loop-like structure apparently erupting from the central few hundred parsecs of our Galaxy. Although its coincidence with the Galactic center has inspired diverse models for its origin, the observational evidence connecting this structure to the GC region has been thin. We describe a multiwavelength observing campaign with the VLA, GBT, Spitzer, and other telescopes that finds compelling evidence that the structure is likely formed by a mass outflow from the central tens of parsecs of our Galaxy. The size and mass

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7

Reich, Wolfgang, Yoshiaki Sofue, and Ernst Fürst. "Thermal and Nonthermal Emission Structures in the Galactic Center Region." Publications of the Astronomical Society of Japan 39, no. 4 (1987): 573–87. https://doi.org/10.1093/pasj/39.4.573.

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Abstract By a detailed comparison of background-filtered maps of the 11-cm (2.695-GHz) radio continuum emission and the 60-μm infrared emission for the central 2° × 3° region of the Galaxy we were able to separate nonthermal and thermal emission structures. Based on this comparison we found that the “galactic center lobe (GCL)” basically has nonthermal characteristics. Near Sgr A two possibly nonthermal spurlike structures are noted. The nuclear disk shows unusual high infrared emission. A previously unrecognized supernova remnant was identified.

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8

Wang, Q. Daniel. "Chandra large-scale mapping of the Galactic Centre: probing high-energy structures around the central molecular zone." Monthly Notices of the Royal Astronomical Society 504, no. 2 (2021): 1609–18. http://dx.doi.org/10.1093/mnras/stab801.

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ABSTRACT Recent observations have revealed interstellar features that apparently connect energetic activity in the central region of our Galaxy to its halo. The nature of these features, however, remains largely uncertain. We present a Chandra mapping of the central 2° × 4° field of the Galaxy, revealing a complex of X-ray-emitting threads plus plume-like structures emerging from the Galactic Centre (GC). This mapping shows that the northern plume or fountain is offset from a well-known radio lobe (or the GCL), which however may represent a foreground H ii region, and that the southern plume i

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9

Shibata, Kazunari, and Yutaka Uchida. "A Magnetodynamical Model for the Galactic Center Lobes." Publications of the Astronomical Society of Japan 39, no. 4 (1987): 559–71. https://doi.org/10.1093/pasj/39.4.559.

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Abstract We present an MHD model for the galactic center lobes (GCL) by using an axisymmetric 2.5-dimensional MHD simulation. According to our model, GCL is a low-energy jet emanating from the H II gas disk extending beyond r ~ 100 pc from the galactic center. The model is based on the “sweeping-magnetic-twist” mechanism developed by the authors for the production of cosmic jets, where the gas in the surface layer of the contracting disk is lifted up by the J × B force in the relaxing magnetic twist, which is generated by the interaction of the rotation of the contracting disk with the poloida

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10

Shibata, Kazunari. "MHD Mechanisms for the Formation of Galactic Center Lobes." Symposium - International Astronomical Union 136 (1989): 313–17. http://dx.doi.org/10.1017/s007418090018667x.

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I critically discuss three possible MHD mechanisms for the formation of Galactic center lobes (GCL) found by Sofue and Handa (1984) from the theoretical point of view. The three mechanisms I shall discuss are: (1) sweeping-magnetic-twist mechanism, (2) explosion in a disk with a vertical magnetic field, and (3) nonlinear Parker instability. I review the characteristics of these mechanisms, which are mainly obtained from nonlinear 2D MHD numerical simulations, and discuss their merits and demerits as possible mechanisms for the formation of GCL and related magnetic structures.

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11

Nicholls, Jennifer, and A. D. Gray. "Modelling the Galactic Centre Snake." Publications of the Astronomical Society of Australia 10, no. 3 (1993): 233–35. http://dx.doi.org/10.1017/s1323358000025741.

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AbstractHigh resolution imaging at radio frequencies has revealed several long, filamentary, non-thermal sources in the Galactic Centre region. One of these, known as the Snake, is unique in that it lies outside the Galactic Centre Lobe, and has two kinks along its length, one of which appears to be associated with a small, resolved source. For this work the Snake is assumed to be embedded in a region where both the magnetic field and the particle energy spectrum are uniform. The Snake is then modelled as an enhancement over the background of the particle energy spectrum. Some preliminary resu

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12

Bally, John. "The Herschel view of the Galactic center." Proceedings of the International Astronomical Union 9, S303 (2013): 1–14. http://dx.doi.org/10.1017/s174392131400009x.

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AbstractThe 3.5 meter diameter Herschel Space Observatory conducted a ∼720 square-degree survey of the Galactic plane, the Herschel Galactic plane survey (Hi-GAL). These data provide the most sensitive and highest resolution observations of the far-IR to sub-mm continuum from the central molecular zone (CMZ) at λ = 70, 160, 250, 350, and 500 μm obtained to date. Hi-GAL can be used to map the distributions of temperature and column density of dust in CMZ clouds, warm dust in Hii regions, and identify highly embedded massive protostars and clusters and the dusty shells ejected by supergiant star

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13

Mirabel, I. F., and O. Laurent. "Feeding the Central Engine in Giant Radio Galaxies." Symposium - International Astronomical Union 194 (1999): 133–39. http://dx.doi.org/10.1017/s0074180900161868.

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Giant radio galaxies are thought to be massive ellipticals powered by accretion of interstellar matter onto a supermassive black hole. Interactions with gas rich galaxies may provide the interstellar matter to feed the active galactic nucleus (AGN). To power radio lobes that extend up to distances of hundreds of kiloparsecs, gas has to be funneled from kiloparsec size scales down to the AGN at rates of ˜1 M⊙ yr−1 during ≥108 years. Therefore, large and massive quasi-stable structures of gas and dust should exist in the deep interior of the giant elliptical hosts of double lobe radio galaxies.

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14

Nagoshi, Halca, Yuzo Kubose, Kenta Fujisawa, et al. "The Galactic center lobe filled with thermal plasma." Publications of the Astronomical Society of Japan 71, no. 4 (2019). http://dx.doi.org/10.1093/pasj/psz060.

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Abstract An observational result of a radio continuum and H92α radio recombination line of the Galactic center lobe (GCL), using the Yamaguchi 32 m radio telescope, is reported. The obtained spatial intensity distribution of the radio recombination line shows two distinctive ridge-like structures extending from the Galactic plane vertically to the north at the eastern and western sides of the Galactic center, which are connected to each other at a latitude of ${1{^{\circ}_{.}}2}$ to form a loop-like structure as a whole. This suggests that most of the radio continuum emission of the GCL is fre

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15

Tsuboi, Masato, Takahiro Tsutsumi, Yoshimi Kitamura, Ryosuke Miyawaki, Atsushi Miyazaki, and Makoto Miyoshi. "Where is the western part of the Galactic Center Lobe located really?" Publications of the Astronomical Society of Japan 72, no. 5 (2020). http://dx.doi.org/10.1093/pasj/psaa077.

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Abstract The Galactic Center Lobe (GCL) is a peculiar object widely protruding from the Galactic plane toward the positive Galactic latitude, which had been found toward the Galactic Center (GC) in the early days of the radio observation. The peculiar shape has suggested a relation with historical events, star burst, large explosion, and so on in the GC. However, the issue of whether the GCL is a single large structure located in the GC region is not yet settled conclusively. In the previous observations, the silhouette against the low-frequency emission was found in the western part of the GC

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16

Soria, Roberto, Ruican Ma, Lian Tao, and Shuang-Nan Zhang. "A 2-hr binary period for the black hole transient MAXI J0637−430." Monthly Notices of the Royal Astronomical Society, July 11, 2022. http://dx.doi.org/10.1093/mnras/stac1896.

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Abstract We revisit various sets of published results from X-ray and optical studies of the Galactic black hole (BH) candidate MAXI J0637−430, which went into outburst in 2019. Combining the previously reported values of peak outburst luminosity, best-fitting radii of inner and outer accretion disk, viewing angle, exponential decay timescale and peak-to-peak separation of the He II λ4686 disk emission line, we improve the constraints on the system parameters. We estimate a heliocentric distance d ≈ (8.7 ± 2.3) kpc, a projected Galactocentric distance R ≈ (13.2 ± 1.8) kpc and a height |z| ≈ (3.

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17

Kumari, Shobha, Sabyasachi Pal, Martin J. Hardcastle, and Maya A. Horton. "J0011+3217: A peculiar radio galaxy with a one-sided secondary lobe and misaligned giant primary lobes." Astronomy & Astrophysics, July 2, 2024. http://dx.doi.org/10.1051/0004-6361/202347367.

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From the LOFAR Two-metre Sky Survey second data release (LoTSS DR2) at 144 MHz, we identified a peculiar radio galaxy, J0011+3217. It has a large, one-sided diffuse secondary wing that stretches up to 0.85 Mpc (roughly 85<!PCT!> of the size of the primary lobe). The linear size of the primary lobe of the galaxy is 0.99 Mpc. This peculiar source is a giant radio galaxy with a misaligned primary lobe. There is an optical galaxy 16 kpc (7 arcsec) from the host active galactic nucleus of J0011+3217. J0011+3217 has a radio luminosity of $1.65 $ W Hz$^ $ at 144 MHz with a spectral index of $-0

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