Update paper.bib (#15)

* Update paper.bib

* Update paper.md

paper/paper.bib

@@ -1,3 +1,45 @@
+@article{Vu:2021coj,
+    author = "Vu, Nils L. and others",
+    title = "{A scalable elliptic solver with task-based parallelism for the SpECTRE numerical relativity code}",
+    eprint = "2111.06767",
+    archivePrefix = "arXiv",
+    primaryClass = "gr-qc",
+    doi = "10.1103/PhysRevD.105.084027",
+    journal = "Phys. Rev. D",
+    volume = "105",
+    number = "8",
+    pages = "084027",
+    year = "2022"
+}
+
+@article{Nee:2024bur,
+    author = "Nee, Peter James and Lara, Guillermo and Pfeiffer, Harald P. and Vu, Nils L.",
+    title = "{Quasistationary hair for binary black hole initial data in scalar Gauss-Bonnet gravity}",
+    eprint = "2406.08410",
+    archivePrefix = "arXiv",
+    primaryClass = "gr-qc",
+    doi = "10.1103/PhysRevD.111.024061",
+    journal = "Phys. Rev. D",
+    volume = "111",
+    number = "2",
+    pages = "024061",
+    year = "2025"
+}
+
+@article{Vu:2024cgf,
+    author = "Vu, Nils L.",
+    title = "{Discontinuous Galerkin scheme for elliptic equations on extremely stretched grids}",
+    eprint = "2405.06120",
+    archivePrefix = "arXiv",
+    primaryClass = "gr-qc",
+    doi = "10.1103/PhysRevD.110.084062",
+    journal = "Phys. Rev. D",
+    volume = "110",
+    number = "8",
+    pages = "084062",
+    year = "2024"
+}
+
 @article{East:2012zn,
     author = "East, William E. and Ramazanoglu, Fethi M. and Pretorius, Frans",
     title = "{Conformal Thin-Sandwich Solver for Generic Initial Data}",

paper/paper.md

@@ -101,7 +101,7 @@ The two main methods for finding initial conditions in numerical relativity are
 ![plot_grtresna](plot.png)
 *Some highlights of work using GRTresna to date: (Left:) Dark matter around binary black holes, from [@Bamber:2022pbs;@Aurrekoetxea:2023jwk;@Aurrekoetxea:2024cqd] (Middle:) Evolution of inflationary perturbations during preheating, from [@Aurrekoetxea:2023jwd]. (Right:) Scalar fields around black holes in* $4\partial ST$ *gravity, from [@Brady:2023dgu]*
 
-# Key features
+# Key features of GRTresna
 
 The key features of GRTresna are as follows
 
@@ -133,8 +133,7 @@ Forthcoming features currently under development include the addition of other m
 # Statement of Need
 
 
-There are a number of existing initial data solvers for numerical relativity, most of which are primarily designed to solve for initial conditions in compact object mergers (i.e. neutron stars and black holes). These include TwoPunctures [@Ansorg:2004ds], SGRID [@Tichy:2009yr], BAM [@Bruegmann:2006ulg], LORENE [@LORENE;@Gourgoulhon:2000nn], Spells [@Pfeiffer:2002wt], COCAL [@Uryu:2011ky;@Tsokaros:2012kp;@Tsokaros:2015fea], PCOCAL [@Boukas:2023ckb], Elliptica [@Rashti:2021ihv], NRPyElliptic [@Assumpcao:2021fhq], KADATH/FUKA [@FUKA;@Grandclement:2009ju;@Papenfort:2021hod}], SPHINCS\_ID [@SPHINCSID;@Diener:2022hui;@Rosswog:2023nnl], and the solver of East *et al.* [@East:2012zn]. Many of these codes, particularly those using spectral methods like TwoPunctures, provide a higher accuracy in the solution compared to GRTresna, which is limited to second order accuracy by the multigrid method used. They are therefore better suited to initial data for waveform generation where precision is key. GRTresna is, however, designed to be more flexible and general purpose, tackling both cosmological and black hole spacetimes in a range of scenarios beyond GR and the Standard Model.
-
+There are a number of existing initial data solvers for numerical relativity, most of which are primarily designed to solve for initial conditions in compact object mergers (i.e. neutron stars and black holes). These include TwoPunctures [@Ansorg:2004ds], SGRID [@Tichy:2009yr], BAM [@Bruegmann:2006ulg], LORENE [@LORENE;@Gourgoulhon:2000nn], Spells [@Pfeiffer:2002wt], SpECTRE [@Vu:2021coj;@Vu:2024cgf] ([@Nee:2024bur] for modified gravity) COCAL [@Uryu:2011ky;@Tsokaros:2012kp;@Tsokaros:2015fea], PCOCAL [@Boukas:2023ckb], Elliptica [@Rashti:2021ihv], NRPyElliptic [@Assumpcao:2021fhq], KADATH/FUKA [@FUKA;@Grandclement:2009ju;@Papenfort:2021hod}], SPHINCS\_ID [@SPHINCSID;@Diener:2022hui;@Rosswog:2023nnl], and the solver of East *et al.* [@East:2012zn]. Many of these codes, particularly those using spectral methods like TwoPunctures and SpECTRE, provide a higher accuracy in the solution compared to GRTresna, which is limited to second order accuracy by the multigrid method used. They are therefore better suited to initial data for waveform generation where precision is key. GRTresna is, however, designed to be more flexible and general purpose, tackling both cosmological and black hole spacetimes in a range of scenarios beyond GR and the Standard Model.
 
 In particular, to the best of our knowledge, there is no fully general, publicly available initial condition solver for inhomogeneous cosmological spacetimes. One exception is FLRWSolver, developed by Macpherson \emph{et al.} [@Macpherson:2016ict] as part of the Einstein Toolkit [@Loffler:2011ay], which specializes in initializing data for cosmological perturbations arising from inflation for studies of late-time cosmology. However, this is limited to only weakly non-linear initial data. GRTresna aims to provide an open-source tool that not only incorporates the general features of existing initial data solvers for compact objects in GR but also extends their capabilities to cosmological spacetimes (see [@Aurrekoetxea:2024mdy] for a review of the application of numerical relativity in cosmology). GRTresna is particularly well-suited for fundamental field matter types, such as scalar and vector fields. Its flexible design allows users to implement new solver methods, additional matter types, or extend the code to study theories beyond GR. It is fully compatible with the GRTL Collaboration's ecosystem of codes but can also serve as a complementary tool for generating constraint-satisfying initial data for other numerical relativity codes.