Capítulo 2. Marco Teórico
2.1. Fundamento teórico
2.1.2. Transferencia de la capacitación
2.1.2.3. Factores que afectan la
XRB populations are important probes of star formation and the physics of binary evolution. Due to the association of XRBs with star clusters and star forming regions, they are intricately linked to how galaxies evolve and allow us to explore the formation of stellar populations. An example is the high-mass end of the stellar initial mass function, which can be investigated because XRB primaries are the endpoints of massive star evolution. However, the faint-end of the XLF, where the majority of sources exist, has yet to be studied in detail beyond the Milky Way.
Low-luminosity X-ray sources represent the next step in understanding XRBs and other
transient systems. With current X-ray telescopes such asChandra, only nearby (large) galax-
ies such as M31 represent realistic targets for examining X-ray sources below luminosities of
∼ 1036 erg s−1. The increase in wide-field surveys across the electromagnetic spectrum, such
as the Panchromatic Hubble Andromeda Treasury Survey (HST; Dalcanton et al. 2012), Next
Generation Virgo Cluster Survey (Canada-France-Hawaii Telescope; Ferrarese et al. 2012),
detailed study of XRBs. Multiwavelength observations are crucial in understanding X-ray
sources, specifically their classification. Radio and γ-ray observations are used in detecting
pulsars while XRB counterparts can be identified and star cluster catalogues constructed with
optical/infrared observations. These types of observations are particularly useful when study-
ing LMXBs and MSPs, especially in GCs. The evolutionary link between LMXBs and MSPs is still not well understood and requires more investigation. Recently, the first binary MSP was identified that was seen to shift between an accretion-powered X-ray state and a rotation- powered radio state (Papitto et al., 2014)[similar work by Patruno et al. (2013)]. This type of behaviour is evidence for an LMXB evolving into a MSP. Monitoring this population for variability can reveal information on accretion disk physics and the evolution of XRBs. Thus an emphasis must be put on exploring XRBs in a quiescent state.
There are still unanswered questions regarding the association of XRBs with different
galaxy environments. We have stated that HMXBs are found at large separations (0.4±0.2 kpc)
from star-forming regions with low significance. This suggests that HMXBs are ejected from their parent environments at birth. Both the spatial and luminosity distributions of HMXBs
below 1036erg s−1have not been studied outside our Galaxy, where the focus has mostly been
on ULXs in starburst galaxies. In addition, the impact of star cluster metallicity on HMXBs is not well understood. However, unlike HMXBs, LMXBs are preferentially found in metal-rich
GCs. The prevalence of LMXBs in metal-rich GCs by a factor of∼3 compared to metal-poor
GCs is astounding for a number of reasons. The effect is independent over the entire range
of bright (> 1036 erg s−1) LMXB luminosity, the GC age, stellar encounter rate, and selection
effects. A plausible explanation for this wide-ranging phenomenon is still needed (Kim et al.,
2013).
Future efforts should therefore comprise studies of quiescent emission in XRB transients
both inside and outside the Milky Way, along with detailed studies of the GC-LMXB metallic-
ity effect. Multiwavelength observations are paramount to advance our understanding of XRBs
clusters and galaxies is complex and requires observations to provide input constraints and a
comparison sample. Tzanavaris et al. (2013) cite deeperChandraobservations as critical for
comparing models to sources with fainter luminosities. XRBs also provide information on the dynamics and evolution of star clusters. Ultimately, the link between XRBs and star clusters is invaluable to studying and achieving a better understanding of both populations.
This thesis focuses on the nature of low-luminosity X-ray sources and the connection be-
tween XRBs and star clusters. Using optical and X-ray data from HSTandChandra, respec-
tively, in our Galaxy and M31, we can probe the faintest sources at both wavelengths and study connections between star cluster and X-ray properties. Our goals are to discover the faintest
extragalactic XRBs in star clusters and explore the GC-LMXB metallicity effect. In Chapter
2, we focus on the star cluster and star-forming environments of M31, and probe the relation- ships between their parameters and X-ray sources at the faintest X-ray luminosities. Chapter 3 presents a detailed X-ray point source catalogue of M31, which is the deepest for any large galaxy outside the Milky Way. In Chapter 4 we study the GC population of our Galaxy to ex- plain the dependence of LMXB formation on metallicity. Chapter 5 summarizes our important conclusions and discusses necessary follow-up as well as other areas of relevant work.
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Chapter 2
X-Rays Beware: The Deepest Chandra
Catalogue of Point Sources in M31
2.1
Executive Summary
This study represents the most sensitiveChandraX-ray point source catalogue of M31. Using
133 publicly available ChandraACIS-I/S observations totalling∼ 1 Ms, we detected 795 X-
ray sources in the bulge, northeast, and southwest fields of M31, covering an area of ≈ 0.6
deg2, to a limiting unabsorbed 0.5−8.0 keV luminosity of∼ 1034 erg s−1. In the inner bulge,
where exposure is approximately constant, X-ray fluxes represent average values because they were determined from many observations over a long period of time. Similarly, our catalogue is more complete in the bulge fields since monitoring allowed more transient sources to be
detected. The catalogue was cross-correlated with a previousXMM-Newtoncatalogue of M31’s
D25 isophote consisting of 1948 X-ray sources, with only 979 within the field of view of our
survey. We found 387 (49%) of ourChandrasources (352 or 44% unique sources) matched to
within 500of 352XMM-Newtonsources. Combining this result with matching done to previous
Chandra X-ray sources we detected 259 new sources in our catalogue. We created X-ray
luminosity functions (XLFs) in the soft (0.5−2.0 keV) and hard (2.0−8.0 keV) bands that are
the most sensitive for any large galaxy based on our detection limits. Completeness-corrected
XLFs show a break around ≈ 1.3× 1037 erg s−1, consistent with previous work. As in past