You signed in with another tab or window. Reload to refresh your session.You signed out in another tab or window. Reload to refresh your session.You switched accounts on another tab or window. Reload to refresh your session.Dismiss alert
Copy file name to clipboardExpand all lines: docs/source/Modeling_without_statistics.ipynb
+1-1Lines changed: 1 addition & 1 deletion
Original file line number
Diff line number
Diff line change
@@ -81,7 +81,7 @@
81
81
"* the [Photosphere](photosphere.rst#xpsi.Photosphere.Photosphere) class;\n",
82
82
"* the [HotRegion](hotregion.rst#xpsi.HotRegion.HotRegion) class;\n",
83
83
"* the [Elsewhere](elsewhere.rst#xpsi.Elsewhere.Elsewhere) class (optionally used in conjuction with HotRegion instances);\n",
84
-
"* the [Everywhere](elsewhere.rst#xpsi.Elsewhere.Elsewhere) class (cannot be used with HotRegion instances);\n",
84
+
"* the [Everywhere](everywhere.rst#xpsi.Everywhere.Everywhere) class (cannot be used with HotRegion instances);\n",
85
85
"* and four low-level user-modifiable routines for evaluation of a parametrised specific intensity model.\n",
86
86
"\n",
87
87
"For this demonstration we will assume that the surface radiation field *elsewhere* (other than the hot regions) can be ignored in the soft X-ray regime our model instrument is sensitive to. We will not be utilizing the [Elsewhere](elsewhere.rst#xpsi.Elsewhere.Elsewhere) class, for which their exists a distinct tutorial (**Global surface emission**). For more advanced modelling, we can simply write custom *derived* classes, and instantiate those derived classes to construct objects for our model. In particular, a common pattern will be to subclass the [HotRegion](hotregion.rst#xpsi.HotRegion.HotRegion) class. Let's start with the [Spacetime](spacetime.rst#xpsi.Spacetime.Spacetime) class."
Copy file name to clipboardExpand all lines: joss/paper.md
+21-35Lines changed: 21 additions & 35 deletions
Display the source diff
Display the rich diff
Original file line number
Diff line number
Diff line change
@@ -39,31 +39,23 @@ affiliations:
39
39
index: 2
40
40
- name: Institut de Recherche en Astrophysique et Planétologie, UPS-OMP, CNRS, CNES, 9 avenue du Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France
41
41
index: 3
42
-
date: 23 September 2022
42
+
date: 26 September 2022
43
43
bibliography: xpsijoss.bib
44
44
---
45
45
46
-
# Summary
47
46
48
-
Stars play host to exotic environments that cannot be simulated in terrestrial
49
-
laboratories. The focus of this work is neutron stars, thought to be the most
50
-
compact extended objects in the Universe. Observable radiation from a neutron
51
-
star encodes information about fundamental physics (gravity, electromagnetism,
52
-
and nuclear forces) and astrophysical processes (such as the state and evolution
53
-
of a stellar magnetosphere). Neutron stars are often detected by astronomers
54
-
because their radiative signal - in radio, X-ray and gamma-rays - is pulsed due to bulk stellar rotation. By modeling the physical process that generates data registered by telescopes, astronomers and astrostatisticians can make inferential statements
55
-
about the nature of the extreme Universe.
47
+
# Summary
56
48
49
+
X-PSI is a software package designed to simulate rotationally-modified (pulsed)
50
+
surface X-ray emission from neutron stars and to perform Bayesian
51
+
statistical inference on real or simulated pulse profile data sets. Model parameters
52
+
of interest include neutron star mass and radius and the system geometry and
53
+
properties of the hot emitting surface regions.
57
54
58
55
# Statement of need
59
56
60
-
There exist open-source libraries and packages to support a subset of the
61
-
modeling treated in astrophysical literature. They provide frameworks,
62
-
toolsets, model implementations, and so on. One sub-field for which there does
63
-
not exist such an open-source project, is for the *statistical modeling* of
64
-
X-ray signals that pulse due to rotational modulation of asymmetric emission
65
-
from the surface of a neutron star. Pulsing X-ray signals from neutron stars
66
-
are modeled to statistically estimate parameters such as stellar mass and
57
+
Rotationally modulated (pulsed) X-ray signals from neutron stars
58
+
can be modeled to statistically estimate parameters such as stellar mass and
67
59
radius, and properties of the surface radiation field such as a map of
68
60
temperature. The mass and radius of a neutron star are a function of the
69
61
equation of state of internal matter (especially the dense matter in the core)
@@ -75,18 +67,15 @@ requires relativistic tracing of radiation as it propagates from surface to a
75
67
distant telescope. Pulse-profile modelling to infer neutron star parameters
76
68
is a major science goal for both current X-ray telescopes such as the Neutron
77
69
Star Interior Composition ExploreR (NICER, @Gendreau2016) and future telescopes
78
-
@Watts2019.
70
+
[@Watts2019].
79
71
80
-
There are a small number of open-source libraries for simulating the X-ray
72
+
While there are some open-source libraries for simulating the X-ray
81
73
signals from rapidly spinning neutron stars and more generally from the
82
-
vicinity of general relativistic compact objects (including black holes).
83
-
An example is the Arcmancer
84
-
library of @Pihajoki:2018, a general purpose toolbox that is wrapped by an
85
-
updated version of the bender library of @Nattila:2016 for the purpose of
86
-
simulating X-ray signals from hot regions on the surfaces of rapidly rotating
87
-
neutron stars. However the scope of these projects does not include statistical modeling, which
74
+
vicinity of general relativistic compact objects including black holes [@Nattila:2016;@Pihajoki:2018] the scope
75
+
of these projects does not include statistical modeling, which
88
76
necessitates tractable parametrised models and a modular framework for
89
-
constructing those models. X-PSI provides this functionality.
77
+
constructing those models. X-PSI addresses this need, coupling code for likelihood
78
+
functionality (simulation) with existing open-source software for posterior sampling (inference).
90
79
91
80
# The X-PSI package and science use
92
81
@@ -112,11 +101,9 @@ integrals at past times normalized to the maximum at each photon energy
0 commit comments