5 research outputs found
A Feminist Analysis of the Changing Roles of Women in Chinua Achebe’s Things Fall Apart and Anthills of the Savannah
No full textChinua Achebe is one of the pioneering figures of African Fiction. In his several critical essays and interviews Achebe has discussed the role of an author belonging to a postcolonial country, and declared that he writes his fiction with a definite role. He has penned five novels including his masterpiece Things Fall Apart (1958) in which Achebe, with his realism, has taken up the task of telling his people the greatness and weaknesses of their Ibo culture. Here, the object of his criticism is the colonizer British exercising power under the guise of a civilizing mission. On the other hand, in one of his most discussed novels Anthills of the Savannah (1987) he takes the role of a conscience builder in a new nation engulfed in cutthroat power politics; and the object of his criticism shifts to his own people, the corrupt educated elite and military officials who have failed to contribute in nation building. However, the role of women in Nigerian society is also one of the prominent issues depicted significantly in both these celebrated novels. The paper focuses on a feminist analysis of these novels with the aim to find out the changing roles of women in Nigerian society depicted in these novels. It takes recourse to the method of explication and close reading of these primary texts and the secondary data in the light of Feminist Criticism.  
The 3XMM/SDSS Stripe 82 Galaxy Cluster Survey - II. X-ray and optical properties of the cluster sample
No full textWe present X-ray and optical properties of the optically confirmed galaxy cluster sample from the 3XMM/SDSS Stripe 82 cluster survey. The sample includes 54 galaxy clusters in the redshift range of 0.05-1.2, with a median redshift of 0.36. We first present the X-ray temperature and luminosity measurements that are used to investigate the X-ray luminosity- temperature relation. The slope and intercept of the relation are consistent with those published in the literature. Then, we investigate the optical properties of the cluster galaxies including their morphological analysis and the galaxy luminosity functions (GLFs). The morphological content of cluster galaxies is investigated as a function of cluster mass and distance from the cluster centre. No strong variation of the fraction of early- and late-type galaxies with cluster mass is observed. The fraction of early-type galaxies as a function of cluster radius varies as expected. The individual GLFs of red sequence galaxies were studied in the five ugriz bands for 48 clusters. The GLFs were then stacked in three mass bins and two redshift bins. Twenty clusters of the present sample are studied for the first time in X-rays, and all are studied for the first time in the optical range. Altogether, our sample appears to have X-ray and optical properties typical of 'average' cluster properties. © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.This work was supported by the Egyptian Science and Technology Development Fund (STDF) and the French Institute in Egypt (IFE) in cooperation with the Institut d'Astrophysique de Paris (IAP), France. FD acknowledges long-term support from the French National Centre for Space Studies (CNES). IM acknowledges support from the Spanish Ministry of Economy and Competitiveness through grants AYA2013-42227-P and AYA2016-76682-C3-1-P.Peer Reviewe
Early-time Observations of SN 2023wrk: A Luminous Type Ia Supernova with Significant Unburned Carbon in the Outer Ejecta
No full textLiu, Jialian et al.--Full list of authors: Liu, Jialian; Wang, Xiaofeng; Andrade, Cristina; Duverne, Pierre-Alexandre; Zhang, Jujia; Li, Liping; Wang, Zhenyu; Navarete, Felipe; Reguitti, Andrea; Schuldt, Stefan; Cai, Yongzhi; Filippenko, Alexei V.; Yang, Yi; Brink, Thomas G.; Zheng, WeiKang; Esamdin, Ali; Iskandar, Abdusamatjan; Bai, Chunhai; Liu, Jinzhong; Li, Xin; Hu, Maokai; Li, Gaici; Li, Wenxiong; Ma, Xiaoran; Yan, Shengyu; Mo, Jun; Adami, Christophe; Akl, Dalya; Antier, Sarah; Broens, Eric; Ducoin, Jean-Grégoire; Elhosseiny, Eslam; Esposito, Thomas M.; Freeberg, Michael; Gokuldass, Priyadarshini; Hello, Patrice; Karpov, Sergey; Márquez, Isabel; Mašek, Martin; Pyshna, Oleksandra; Rajabov, Yodgor; Saint-Gelais, Denis; Serrau, Marc; Sokoliuk, Oleksii; Takey, Ali; Tanasan, Manasanun; Turpin, DamienWe present extensive photometric and spectroscopic observations of the nearby Type Ia supernova (SN) 2023wrk at a distance of about 40 Mpc. The earliest detection of this SN can be traced back to a few hours after the explosion. Within the first few days, the light curve shows a bump feature, while the B − V color is blue and remains nearly constant. The overall spectral evolution is similar to that of an SN 1991T/SN 1999aa-like SN Ia, while the C iiλ6580 absorption line appears to be unusually strong in the first spectrum taken at t ≈ −15.4 days after the maximum light. This carbon feature disappears quickly in subsequent evolution but it reappears at around the time of peak brightness. The complex evolution of the carbon line and the possible detection of Ni iii absorption around 4700 Å and 5300 Å in the earliest spectra indicate macroscopic mixing of fuel and ash. The strong carbon lines are likely related to the collision of SN ejecta with unbound carbon, consistent with the predictions of pulsational delayed-detonation or carbon-rich circumstellar-matter interaction models. Among those carbon-rich SNe Ia with strong C iiλ6580 absorption at very early times, the line-strength ratio of C ii to Si ii and the B − V color evolution are found to exhibit large diversity, which may be attributed to different properties of unbound carbon and outward-mixing 56Ni. © 2024. The Author(s). Published by the American Astronomical Society.This work is supported by the National Natural Science Foundation of China (NSFC grants 12288102, 12033003, and 12090044) and the Tencent Xplorer Prize. J.Z.L is supported by the Tianshan Talent Training Program through grant 2023TSYCCX0101. J.-J.Z. and Y.-Z.C. are supported by the International Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). J.-J.Z. is supported by the National Key R&D Program of China (No. 2021YFA1600404), NSFC grant 12173082, the Yunnan Province Foundation (grant 202201AT070069), the Top-notch Young Talents Program of Yunnan Province, and the Light of West China Program provided by the Chinese Academy of Sciences. Y.-Z.C. is supported by NSFC grant 12303054 and Yunnan Fundamental Research Projects grant 202401AU070063. A.V.F.'s group at UC Berkeley received financial assistance from the Christopher R. Redlich Fund, as well as donations from Gary and Cynthia Bengier, Clark and Sharon Winslow, Alan Eustace, William Draper, Timothy and Melissa Draper, Briggs and Kathleen Wood, and Sanford Robertson (W.Z. is a Bengier–Winslow–Eustace Specialist in Astronomy, T.G.B. is a Draper–Wood–Robertson Specialist in Astronomy, Y.Y. was a Bengier–Winslow–Robertson Fellow in Astronomy), and numerous other donors. X.L. is supported by the Innovation Project of Being Academy of Science and Technology (24CD013). A.R. acknowledges financial support from the GRAWITA Large Program Grant (PI P. D'Avanzo) and the PRIN-INAF 2022 program "Shedding light on the nature of gap transients: from the observations to the models." I.M. is grateful for support from Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033. The work of F.N. is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. W. Corradi is supported by Laboratório Nacional de Astrofísica (LNA) through project numbers P-003, P-011, I-004, and I-013 from OPD. The work of L. de Almeida is supported by Laboratório Nacional de Astrofísica (LNA) through project numbers I-009, I-022, I-027, and P-008 from OPD. N. Sasaki is supported by Universidade do Estado do Amazonas—UEA and LNA through project numbers P-003, P-008, I-004, and I-007. This work is supported by CNRS-MITI and Programme National des Hautes Energies (PNHE). We thank the staffs at the various observatories where data were obtained. A major upgrade of the Kast spectrograph on the Shane 3 m telescope at Lick Observatory, led by Brad Holden, was made possible through generous gifts from the Heising-Simons Foundation, William and Marina Kast, and the University of California Observatories. Research at Lick Observatory is partially supported by a generous gift from Google. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA-CSIC) under a joint agreement with the University of Copenhagen and NOT. This work is partially based on observations collected with the Copernico 1.82 m telescope and the Schmidt 67/92 telescope (Asiago Mount Ekar, Italy) of the INAF—Osservatorio Astronomico di Padova. We thank Stefan Taubenberger and his group of students from MPA for an epoch of ALFOSC imaging and a spectrum taken during a run for educational observations at the 1.82 m Copernico telescope. Part of the photometric data of this work were obtained by the Nanshan One-meter Wide-field Telescope, which is supported by Tianshan Talent Training Program (grant 2023TSYCLJ0053) and the National Key R&D program of China for Intergovernmental Scientific and Technological Innovation Cooperation Project under grant 2022YFE0126200. We acknowledge the support of the staff of the Xinglong 80 cm telescope (TNT). This work was partially supported by the Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences. This research was partially based on observations made with the Thai Robotic Telescope under program ID TRTToO_2024001 and TRTC11B_002, which is operated by the National Astronomical Research Institute of Thailand (Public Organization). The ZTF forced-photometry service was funded under Heising-Simons Foundation grant 12540303 (PI M. Graham). This work makes use of the NASA/IPAC Extragalactic Database (NED), which is funded by NASA and operated by the California Institute of Technology. This article is based in part on observations made at the Observatorios de Canarias del IAC with the TNG telescope operated on the island of La Palma by the Fundación Galileo Galilei INAF, Fundación Canaria (FGG), in the Observatorio del Roque de los Muchachos (ORM). The operation of FRAM telescopes is supported by grants of the Ministry of Education of the Czech Republic LM2023032 and LM2023047, as well as EU/MEYS grants CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/18_046/0016007, CZ.02.1.01/0.0/0.0/ 16_019/0000754, and CZ.02.01.01/00/22_008/0004632. NRIAG team acknowledges financial support from the Egyptian Science, Technology & Innovation Funding Authority (STDF) under grant number 45779. Based in part on observations made at Observatoire de Haute Provence (CNRS), France, with the MISTRAL instrument. This research has also made use of the MISTRAL database, operated at CeSAM (LAM), Marseille, France. We acknowledge the excellent support from Observatoire de Haute-Provence, in particular Jerome Schmitt, Jean Claude Brunel, Francois Huppert, Jean Balcaen, Yoann Degot-Longhi, Stephane Favard, and Jean-Pierre Troncin. We thank the OHP director for the allocations of two DDT observing slots. The work of K. Noysena and M. Tanasan is based on observations made with the Thai Robotic Telescope under program ID TRTC11A_003, which is operated by the National Astronomical Research Institute of Thailand (Public Organization). We acknowledge resources at IJCLAB for hosting science portals and data-reduction pipelines thanks to J. Peloton.
We acknowledge major contributions from the GRANDMA Collaboration and the Kilonova-Catcher citizen science program for the photometric and spectroscopic observations taken over 3 months and their subsequent data reduction. The authors express special gratitude to the PI of GRANDMA and the core team who decided to allocate substantial resources of the collaboration to the study of SN 2023wrk (S. Antier, D. Turpin, I. Tosta e Melo, M. Coughlin, P. Hello, P.-A. Duverne, S. Karpov, T. Pradier, J. Peloton, A. Klotz, C. Andrade). We thank observers of the GRANDMA network program who actively participated in the follow-up campaign: AbAO observatory (N. Kochiashvili, R. Inasaridze and V. Aivazyan) for 1 observation; ShAO Observatory (N. Ismailov, Z. Vidadi, S. Aghayeva, S. Alishov, E. Hesenov) for 3 observations; HAO telescopes (A. Kaeouach) for 12 observations; FRAM telescopes (M. Mašek and S. Karpov) for 194 observations; KAO telescope (E. G. Elhosseiny, M. Abdelkareem, A. Takey, R. H. Mabrouk, A. Shokry, M. Aboueisha, Y. Hendy, A. E. Abdelaziz, R. Bendary, I. Zead, T. M. Kamel, G. M. Hamed, S. A. Ata, W. A. Badawy) for 67 observations; TRT (K. Noysena, M. Tanasan) for 3 observations; and TBC, UBAI telescopes (Y. Tillayev, O. Burkhonov, Sh. Ehgamberdiev, Y. Rajabov) for 9 observations. We acknowledge operations within GRANDMA with crucial participation of 22 follow-up advocates (C. Andrade, P. Gokuldass, M. Tanasan, I. Abdi, D. Akl, P. Hello, O. Pyshna, A. Simon, J-G. Ducoin, Y. Tillayev, M. Mašek, Z. Vidadi, Y. Rajabov, S. Antier, T. Leandro de Almeida, F. Navarete, N. Sasaki, W. Corradi, I. Tosta e Melo, M. Coughlin, T. Hussenot-Desenonges, S. Aghayeva) and their leaders (C. Andrade, P. Hello, S. Antier, I. Tosta e Melo), who participated in providing adequate observation strategies. We thank the whole Data Analysis Group of GRANDMA consisting of I. Abdi, D. Akl, C. Andrade, J.-G. Ducoin, P.-A. Duverne, S. Karpov, F. Navarete, and D. Turpin. P.-A. Duverne is grateful to Etienne Bertrand and Emmanuel Soubrouillard for providing the source's spectra and their help in analyzing these data. D. Turpin, PI of the Kilonova-Catcher, acknowledges the observers of the Kilonova-Catcher program who actively participated in the follow-up campaign: E. Broens,F. Dubois, M. Freeberg, C. Galdies, R. Kneip, D. Marchais, E. Maris, R. Ménard, M. Odeh, G. Parent, A. Popowicz, D. ST-Gelais, and M. Serrau. We also thank Unistellar observers B. Guillet, B. Haremza, G. Di Tommaso, K. Borrot, M. Lorber, M. Shimizu, M. Mitchell, N. Meneghelli, N. Delaunoy, O. Clerget, P. Huth, P. Heafner, P. Kuossari, S. Saibi, S. Price, W. Ono, and Y. Arnaud.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).Peer reviewe
Multiband Optical Variability of the Blazar 3C 454.3 on Diverse Timescales
No full textDue to its peculiar and highly variable nature, the blazar 3C 454.3 has been extensively monitored by the WEBT team. Here, we present for the first time these long-term optical flux and color variability results using data acquired in B, V, R, and I bands over a time span of about two decades. We include data from WEBT collaborators and public archives such as SMARTS, Steward Observatory, and Zwicky Transient Facility. The data are binned and segmented to study the source over this long term when more regular sampling was available. During our study, the long-term spectral variability reveals a redder-when-brighter trend, which, however, stabilizes at a particular brightness cutoff of ∼14.5 mag in the I band, after which it saturates and evolves into a complex state. This trend indicates increasing dominance of jet emission over accretion disk (AD) emission until jet emission completely dominates. Plots of the variation in spectral index (following Fν ∝ ν−α) reveal a bimodal distribution using a one-day binning. These correlate with two extreme phases of 3C 454.3, an outburst or high-flux state and a quiescent or low-flux state, which are respectively jet- and AD-dominated. We have also conducted intraday variability studies of nine light curves and found that six of them are variable. Discrete correlation function analysis between different pairs of optical wave bands peaks at zero lags, indicating cospatial emission in different optical bands. © 2024. The Author(s). Published by the American Astronomical Society
Multiband analyses of the bright GRB 230812B and the associated SN2023pel
No full textHussenot-Desenonges, T. et al.-- Full list of authors: Hussenot-Desenonges, T.; Wouters, T.; Guessoum, N.; Abdi, I.; Abulwfa, A.; Adami, C.; Agüí Fernández, J. F.; Ahumada, T.; Aivazyan, V.; Akl, D.; Anand, S.; Andrade, C. M.; Antier, S.; Ata, S. A.; D'Avanzo, P.; Azzam, Y. A.; Baransky, A.; Basa, S.; Blazek, M.; Bendjoya, P.; Beradze, S.; Boumis, P.; Bremer, M.; Brivio, R.; Buat, V.; Bulla, M.; Burkhonov, O.; Burns, E.; Cenko, S. B.; Coughlin, M. W.; Corradi, W.; Daigne, F.; Dietrich, T.; Dornic, D.; Ducoin, J. -G.; Duverne, P. -A.; Elhosseiny, E. G.; Elnagahy, F. I.; El-Sadek, M. A.; Ferro, M.; Le Floc'h, E.; Freeberg, M.; Fynbo, J. P. U.; Götz, D.; Gurbanov, E.; Hamed, G. M.; Hasanov, E.; Healy, B. F.; Heintz, K. E.; Hello, P.; Inasaridze, R.; Iskandar, A.; Ismailov, N.; Izzo, L.; Jhawar, S.; Jegou du Laz, T.; Kamel, T. M.; Karpov, S.; Klotz, A.; Koulouridis, E.; Kuin, N. P.; Kochiashvili, N.; Leonini, S.; Lu, K. -X.; Malesani, D. B.; Mašek, M.; Mao, J.; Melandri, A.; Mihov, B. M.; Natsvlishvili, R.; Navarete, F.; Nedora, V.; Nicolas, J.; Odeh, M.; Palmerio, J.; Pang, P. T. H.; De Pasquale, M.; Peng, H. W.; Pormente, S.; Peloton, J.; Pradier, T.; Pyshna, O.; Rajabov, Y.; Rakotondrainibe, N. A.; Rivet, J. -P.; Rousselot, L.; Saccardi, A.; Sasaki, N.; Schneider, B.; Serrau, M.; Shokry, A.; Slavcheva-Mihova, L.; Simon, A.; Sokoliuk, O.; Srinivasaragavan, G.; Strausbaugh, R.; Takey, A.; Tanvir, N. R.; Thöne, C. C.; Tillayev, Y.; Tosta e Melo, I.; Turpin, D.; de Ugarte Postigo, A.; Vasylenko, V.; Vergani, S. D.; Vidadi, Z.; Xu, D.; Wang, L. T.; Wang, X. F.; Winters, J. M.; Zhang, X. -L.; Zhu, Z.GRB 230812B is a bright and relatively nearby (z = 0.36) long gamma-ray burst (GRB) that has generated significant interest in the community and has thus been observed over the entire electromagnetic spectrum. We report over 80 observations in X-ray, ultraviolet, optical, infrared, and submillimetre bands from the GRANDMA (Global Rapid Advanced Network for Multimessenger Addicts) network of observatories and from observational partners. Adding complementary data from the literature, we then derive essential physical parameters associated with the ejecta and external properties (i.e. the geometry and environment) of the GRB and compare with other analyses of this event. We spectroscopically confirm the presence of an associated supernova, SN2023pel, and we derive a photospheric expansion velocity of v ∼ 17 × 10 km s. We analyse the photometric data first using empirical fits of the flux and then with full Bayesian inference. We again strongly establish the presence of a supernova in the data, with a maximum (pseudo-)bolometric luminosity of 5.75 × 10 erg s, at 15.76 d (in the observer frame) after the trigger, with a half-max time width of 22.0 d. We compare these values with those of SN1998bw, SN2006aj, and SN2013dx. Our best-fitting model favours a very low density environment (log(n/cm) = -2.38) and small values for the jet's core angle θ = 1.54 deg and viewing angle θ = 0.76 deg. GRB 230812B is thus one of the best observed afterglows with a distinctive supernova bump. © 2024 The Author(s).This work has been coordinated with Mansi Kasliwal and Brad
Cenko’s group, with whom we shared common developments and
visions for time-domain astronomy tools and methods (e.g. SKYPORTAL). We thank Gokul Prem Srinivasaragavan in particular for fruitful
exchanges on this object. We also thank the anonymous reviewer for
constructive comments that have helped improve the paper. The GRANDMA collaboration thanks its entire network of observatories/observers, all its partners in observations and analyses, and
the amateur participants of its Kilonova-Catcher (KNC) programme.
We dedicate this work to D. A. Kann, whose groundbreaking work
in the field of GRBs earned him international recognition over the
past two decades. Alex, your contributions to the world of GRB
science will always be remembered. We deeply miss you and hope
you are proud of the way the GRB community carries on your legacy.
This research has also made use of the MISTRAL data base, based
on observations made at Observatoire de Haute Provence (CNRS),
France, with the MISTRAL spectro-imager, and operated at CeSAM
(LAM), Marseille, France. The GRB OHP observing team is particularly grateful to Jerome ´ Schmitt for the major role he has played
in the development and operations of the MISTRAL instrument at
the T193 telescope. GRANDMA thanks amateur astronomers for
their observations: MS, KF, SL, JN, MF, MO. This work is based on
observations carried out under project number S23BG with the IRAM
NOEMA interferometer. Partly based on observations made with the
Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof´ısica de
Canarias, on the island of La Palma. Partly based on observations
made with the Nordic Optical Telescope, owned in collaboration by
the University of Turku and Aarhus University, and operated jointly
by Aarhus University, the University of Turku, and the University
of Oslo, representing Denmark, Finland, and Norway, the University
of Iceland and Stockholm University at the Observatorio del Roque
de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica
de Canarias. This work is based on observations collected at the
Centro Astronomico ´ Hispano en Andaluc´ıa (CAHA) at Calar Alto,
operated jointly by Junta de Andaluc´ıa and Consejo Superior de
Investigaciones Cient´ıficas (IAA-CSIC) (Programme code: 23B2.2-24, PI Agu¨´ı Fernandez, ´ J. F.). This work used Expanse at the
San Diego Supercomputer Cluster through allocation AST200029 –
‘Towards a complete catalog of variable sources to support efficient
searches for compact binary mergers and their products’ from the
Advanced Cyberinfrastructure Coordination Ecosystem: Services &
Support (ACCESS) programe. WC and NS wish to thank Laboratorio ´
Nacional de Astrof´ısica – LNA and OPD staff, Universidade do
Estado do Amazonas – UEA and the Brazilian Agencies CNPq and
Capes.
GRANDMA has received financial support from the CNRS
through the MITI interdisciplinary programmes. TW and PTHP
are supported by the research programme of the Netherlands
Organization for Scientific Research (NWO). SA acknowledges
the financial support of the Programme National Hautes Energies
(PNHE). MWC acknowledges support from the National Science
Foundation with grant numbers PHY-2347628 and OAC-2117997.
CA and MWC were supported by the Preparing for Astrophysics
with LSST Program, funded by the Heising-Simons Foundation
through grant 2021–2975, and administered by Las Cumbres
Observatory. The Egyptian team acknowledges support from the
Science, Technology & Innovation Funding Authority (STDF) under
grant number 45779. SK is supported by European Structural and
Investment Fund and the Czech Ministry of Education, Youth and
Sports (Project CoGraDS – CZ.02.1.01/0.0/0.0/15 003/0000437).
NPMK is supported by the UKSA Swift operations grant. NG,
DA, and IA acknowledge support from the American University of
Sharjah (UAE) through the grant FRG22-C-S68. MM issupported by
the LM2023032 and LM2023047 grants of the Ministry of Education
of the Czech Republic. JM is supported by the National Key R & D
Program of China (2023YFE0101200), the Yunnan Revitalization
Talent Support Program (YunLing Scholar Award), and NSFC grant
12393813. DBM acknowledgessupport from the European Research
Council (ERC) under the European Union’s research and innovation
programme (ERC Grant HEAVYMETAL No. 101071865). JGD is
supported by a research grant from the Ile-de-France Region within
the framework of the Domaine d’Inter´ etˆ Majeur-Astrophysique et
Conditions d’Apparition de la Vie (DIM-ACAV). The work of FN
is supported by NOIRLab, which is managed by the Association
of Universities for Research in Astronomy (AURA) under a
cooperative agreement with the National Science Foundation. The
Kilonova-Catcher programme is supported by the IdEx Universite´
de Paris Cite,´ ANR-18-IDEX-0001 and Paris-Saclay, IJCLAB.
IRAM is supported by INSU/CNRS (France), MPG (Germany) and
IGN (Spain). The Cosmic Dawn Center is supported by the Danish
National Research Foundation. The Advanced Cyberinfrastructure
Coordination Ecosystem: Services & Support (ACCESS) programe
is supported by National Science Foundation grants #2138259,
#2138286, #2138307, #2137603, and #2138296. With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S)
