Isolated massive stars in the Galactic center: The dynamic contribution from the Arches and Quintuplet star clusters

Habibi, M.; Stolte, A.; Harfst, Stefan

doi:10.1051/0004-6361/201323030

Cited by 45 publications

(50 citation statements)

References 70 publications

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“…Such structures have been observed for globular clusters and have yielded insight into the object's orbit and the gravitational potential of the Galaxy (e.g., Odenkirchen et al 2001Odenkirchen et al , 2003Grillmair & Johnson 2006). Adopting the model of the initial conditions of the Arches from Harfst et al (2010), adopting the 3D velocity from Clarkson et al (2012), and assuming a current position 100 pc in front of the GC, Habibi et al (2014) predict that the Arches should have tidal tails extending 20 pc (∼500″) along the Galactic plane. To search for these structures, we compare the radial profiles parallel and perpendicular to the cluster's bulk velocity, which is consistent with the direction of the Galactic plane (Clarkson et al 2012).…”

Section: The Search For Tidal Tailsmentioning

confidence: 99%

The Arches Cluster: Extended Structure and Tidal Radius

Hosek

Anderson

et al. 2015

ApJ

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At a projected distance of ∼26 pc from Sgr A * , the Arches cluster provides insight into star formation in the extreme Galactic center (GC) environment. Despite its importance, many key properties, such as the cluster's internal structure and orbital history, are not well known. We present an astrometric and photometric study of the outer region of the Arches cluster (R > 6 25) using Hubble Space Telescope WFC3IR. Using proper motions, we calculate membership probabilities for stars down to F153M = 20 mag (∼2.5 M e ) over a 120″ × 120″ field of view, an area 144 times larger than previous astrometric studies of the cluster. We construct the radial profile of the Arches to a radius of 75″ (∼3 pc at 8 kpc), which can be well described by a single power law. From this profile we place a 3σ lower limit of 2.8 pc on the observed tidal radius, which is larger than the predicted tidal radius (1-2.5 pc). Evidence of mass segregation is observed throughout the cluster, and no tidal tail structures are apparent along the orbital path. The absence of breaks in the profile suggests that the Arches has not likely experienced its closest approach to the GC between ∼0.2 and 1 Myr ago. If accurate, this constraint indicates that the cluster is on a prograde orbit and is located in front of the sky plane that intersects Sgr A * . However, further simulations of clusters in the GC potential are required to interpret the observed profile with more confidence.

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Section: The Search For Tidal Tailsmentioning

confidence: 99%

The Arches Cluster: Extended Structure and Tidal Radius

Hosek

Anderson

et al. 2015

ApJ

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“…For a typical neutron star kick velocity, PSR J1746−2850 could have reached its radio position in its short lifetime (Deneva et al 2009). Alternatively, the progenitor star itself could have been stripped from one of the clusters and would have had more time to travel to the observed radio position (Habibi et al 2014). If the source again rebrightens in the radio, its proper motion should be measurable and could distinguish between these scenarios.…”

Section: Gc Star Formationmentioning

confidence: 99%

A transient, flat spectrum radio pulsar near the Galactic Centre

Dexter¹,

Degenaar²,

Kerr³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Recent studies have shown possible connections between highly magnetized neutron stars ("magnetars"), whose X-ray emission is too bright to be powered by rotational energy, and ordinary radio pulsars. In addition to the magnetar SGR J1745−2900, one of the radio pulsars in the Galactic centre (GC) region, PSR J1746−2850, had timing properties implying a large magnetic field strength and young age, as well as a flat spectrum. All characteristics are similar to those of rare, transient, radio-loud magnetars. Using several deep non-detections from the literature and two new detections, we show that this pulsar is also transient in the radio. Both the flat spectrum and large amplitude variability are inconsistent with the light curves and spectral indices of 3 radio pulsars with high magnetic field strengths. We further use frequent, deep archival imaging observations of the GC in the past 15 years to rule out a possible X-ray outburst with a luminosity exceeding the rotational spin down rate. This source, either a transient magnetar without any detected X-ray counterpart or a young, strongly magnetized radio pulsar producing magnetar-like radio emission, further blurs the line between the two categories. We discuss the implications of this object for the radio emission mechanism in magnetars and for star and compact object formation in the GC.

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“…Around 1/3 of these sources are located outside of the three massive startburst cluster suggesting the evidence of isolated high mass stars formation in the GC. However these isolated stars could have been kicked out from the Arches or the Quintuplet cluster due to their dynamics [12]. The Arches cluster seems too young to have supernovae.…”

Section: Cr Injection: Single or Multiple Accelerators ?mentioning

confidence: 99%

Origin of cosmic rays excess in the Galactic Center

Jouvin¹,

Lemière²,

Terrier³

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The center of our Galaxy hosts a Super-Massive Black Hole (SMBH) of about 4× 10 6 M sun . Since it has been argued that the SMBH might accelerate particles up to very high energies, its current and past activity could contribute to the population of Galactic cosmic-rays (CRs). Additionally, the condition in the Galactic Center (GC) are often compared with the one of a starburst system. The high supernovae (SN) rate associated with the strong massive star formation in the region must create a sustained CR injection in the GC via the shocks produced at the time of their explosion. Indeed, the presence of an excess of very high energy (VHE) cosmic rays in the inner 100 pc of the Galaxy has been revealed in 2006 by the H.E.S.S. collaboration. On very large scale (≈ 10 kpc), the non-thermal signature of the escaping GC cosmic rays could have been detected recently as the spectacular "Fermi bubbles". The origin of the CRs over-abundance in the GC still remains mysterious: Is it due to a single impulsive or stationary accelerator at the center or to multiple accelerators filling the region? In order to answer these questions, we build a 3D model of CR injection and propagation with a realistic 3D gas distribution. We then compare with existing data of H.E.S.S.. We discuss the CR injection in the region by a spectral and morphology comparison. We place constrains on the SNR rate and on the diffusion parameters.

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Isolated massive stars in the Galactic center: The dynamic contribution from the Arches and Quintuplet star clusters

Cited by 45 publications

References 70 publications

The Arches Cluster: Extended Structure and Tidal Radius

The Arches Cluster: Extended Structure and Tidal Radius

A transient, flat spectrum radio pulsar near the Galactic Centre

Origin of cosmic rays excess in the Galactic Center

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