Observational constraints on cosmological future singularities

Abstract In this work we consider a family of cosmological models featuring future singularities. This type of cosmological evolution is typical of dark energy models with an equation of state violating some of the standard energy conditions (e.g. the null energy condition). Such a kind of behavior,...
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Autor*in:	Beltrán Jiménez, Jose [verfasserIn] Lazkoz, Ruth [verfasserIn] Sáez-Gómez, Diego [verfasserIn] Salzano, Vincenzo [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2016

Schlagwörter:	Dark Energy Dark Energy Model Effective Field Theory Null Energy Condition Future Singularity

Übergeordnetes Werk:	Enthalten in: The European physical journal - Berlin : Springer, 1998, 76(2016), 11 vom: 19. Nov.
Übergeordnetes Werk:	volume:76 ; year:2016 ; number:11 ; day:19 ; month:11

Links:	Volltext

DOI / URN:	10.1140/epjc/s10052-016-4470-5

Katalog-ID:	SPR008348944

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allfields	10.1140/epjc/s10052-016-4470-5 doi (DE-627)SPR008348944 (SPR)s10052-016-4470-5-e DE-627 ger DE-627 rakwb eng 530 ASE 33.50 bkl Beltrán Jiménez, Jose verfasserin aut Observational constraints on cosmological future singularities 2016 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In this work we consider a family of cosmological models featuring future singularities. This type of cosmological evolution is typical of dark energy models with an equation of state violating some of the standard energy conditions (e.g. the null energy condition). Such a kind of behavior, widely studied in the literature, may arise in cosmologies with phantom fields, theories of modified gravity or models with interacting dark matter/dark energy. We briefly review the physical consequences of these cosmological evolution regarding geodesic completeness and the divergence of tidal forces in order to emphasize under which circumstances the singularities in some cosmological quantities correspond to actual singular spacetimes. We then introduce several phenomenological parameterizations of the Hubble expansion rate to model different singularities existing in the literature and use SN Ia, BAO and H(z) data to constrain how far in the future the singularity needs to be (under some reasonable assumptions on the behavior of the Hubble factor). We show that, for our family of parameterizations, the lower bound for the singularity time cannot be smaller than about 1.2 times the age of the universe, what roughly speaking means %${\sim }2.8%$ Gyrs from the present time. Dark Energy (dpeaa)DE-He213 Dark Energy Model (dpeaa)DE-He213 Effective Field Theory (dpeaa)DE-He213 Null Energy Condition (dpeaa)DE-He213 Future Singularity (dpeaa)DE-He213 Lazkoz, Ruth verfasserin aut Sáez-Gómez, Diego verfasserin aut Salzano, Vincenzo verfasserin aut Enthalten in The European physical journal Berlin : Springer, 1998 76(2016), 11 vom: 19. Nov. (DE-627)253722934 (DE-600)1459069-4 1434-6052 nnns volume:76 year:2016 number:11 day:19 month:11 https://dx.doi.org/10.1140/epjc/s10052-016-4470-5 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2031 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2061 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2113 GBV_ILN_2119 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 33.50 ASE AR 76 2016 11 19 11
spelling	10.1140/epjc/s10052-016-4470-5 doi (DE-627)SPR008348944 (SPR)s10052-016-4470-5-e DE-627 ger DE-627 rakwb eng 530 ASE 33.50 bkl Beltrán Jiménez, Jose verfasserin aut Observational constraints on cosmological future singularities 2016 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In this work we consider a family of cosmological models featuring future singularities. This type of cosmological evolution is typical of dark energy models with an equation of state violating some of the standard energy conditions (e.g. the null energy condition). Such a kind of behavior, widely studied in the literature, may arise in cosmologies with phantom fields, theories of modified gravity or models with interacting dark matter/dark energy. We briefly review the physical consequences of these cosmological evolution regarding geodesic completeness and the divergence of tidal forces in order to emphasize under which circumstances the singularities in some cosmological quantities correspond to actual singular spacetimes. We then introduce several phenomenological parameterizations of the Hubble expansion rate to model different singularities existing in the literature and use SN Ia, BAO and H(z) data to constrain how far in the future the singularity needs to be (under some reasonable assumptions on the behavior of the Hubble factor). We show that, for our family of parameterizations, the lower bound for the singularity time cannot be smaller than about 1.2 times the age of the universe, what roughly speaking means %${\sim }2.8%$ Gyrs from the present time. Dark Energy (dpeaa)DE-He213 Dark Energy Model (dpeaa)DE-He213 Effective Field Theory (dpeaa)DE-He213 Null Energy Condition (dpeaa)DE-He213 Future Singularity (dpeaa)DE-He213 Lazkoz, Ruth verfasserin aut Sáez-Gómez, Diego verfasserin aut Salzano, Vincenzo verfasserin aut Enthalten in The European physical journal Berlin : Springer, 1998 76(2016), 11 vom: 19. Nov. (DE-627)253722934 (DE-600)1459069-4 1434-6052 nnns volume:76 year:2016 number:11 day:19 month:11 https://dx.doi.org/10.1140/epjc/s10052-016-4470-5 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2031 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2061 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2113 GBV_ILN_2119 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 33.50 ASE AR 76 2016 11 19 11
allfields_unstemmed	10.1140/epjc/s10052-016-4470-5 doi (DE-627)SPR008348944 (SPR)s10052-016-4470-5-e DE-627 ger DE-627 rakwb eng 530 ASE 33.50 bkl Beltrán Jiménez, Jose verfasserin aut Observational constraints on cosmological future singularities 2016 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In this work we consider a family of cosmological models featuring future singularities. This type of cosmological evolution is typical of dark energy models with an equation of state violating some of the standard energy conditions (e.g. the null energy condition). Such a kind of behavior, widely studied in the literature, may arise in cosmologies with phantom fields, theories of modified gravity or models with interacting dark matter/dark energy. We briefly review the physical consequences of these cosmological evolution regarding geodesic completeness and the divergence of tidal forces in order to emphasize under which circumstances the singularities in some cosmological quantities correspond to actual singular spacetimes. We then introduce several phenomenological parameterizations of the Hubble expansion rate to model different singularities existing in the literature and use SN Ia, BAO and H(z) data to constrain how far in the future the singularity needs to be (under some reasonable assumptions on the behavior of the Hubble factor). We show that, for our family of parameterizations, the lower bound for the singularity time cannot be smaller than about 1.2 times the age of the universe, what roughly speaking means %${\sim }2.8%$ Gyrs from the present time. Dark Energy (dpeaa)DE-He213 Dark Energy Model (dpeaa)DE-He213 Effective Field Theory (dpeaa)DE-He213 Null Energy Condition (dpeaa)DE-He213 Future Singularity (dpeaa)DE-He213 Lazkoz, Ruth verfasserin aut Sáez-Gómez, Diego verfasserin aut Salzano, Vincenzo verfasserin aut Enthalten in The European physical journal Berlin : Springer, 1998 76(2016), 11 vom: 19. Nov. (DE-627)253722934 (DE-600)1459069-4 1434-6052 nnns volume:76 year:2016 number:11 day:19 month:11 https://dx.doi.org/10.1140/epjc/s10052-016-4470-5 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2031 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2061 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2113 GBV_ILN_2119 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 33.50 ASE AR 76 2016 11 19 11
allfieldsGer	10.1140/epjc/s10052-016-4470-5 doi (DE-627)SPR008348944 (SPR)s10052-016-4470-5-e DE-627 ger DE-627 rakwb eng 530 ASE 33.50 bkl Beltrán Jiménez, Jose verfasserin aut Observational constraints on cosmological future singularities 2016 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In this work we consider a family of cosmological models featuring future singularities. This type of cosmological evolution is typical of dark energy models with an equation of state violating some of the standard energy conditions (e.g. the null energy condition). Such a kind of behavior, widely studied in the literature, may arise in cosmologies with phantom fields, theories of modified gravity or models with interacting dark matter/dark energy. We briefly review the physical consequences of these cosmological evolution regarding geodesic completeness and the divergence of tidal forces in order to emphasize under which circumstances the singularities in some cosmological quantities correspond to actual singular spacetimes. We then introduce several phenomenological parameterizations of the Hubble expansion rate to model different singularities existing in the literature and use SN Ia, BAO and H(z) data to constrain how far in the future the singularity needs to be (under some reasonable assumptions on the behavior of the Hubble factor). We show that, for our family of parameterizations, the lower bound for the singularity time cannot be smaller than about 1.2 times the age of the universe, what roughly speaking means %${\sim }2.8%$ Gyrs from the present time. Dark Energy (dpeaa)DE-He213 Dark Energy Model (dpeaa)DE-He213 Effective Field Theory (dpeaa)DE-He213 Null Energy Condition (dpeaa)DE-He213 Future Singularity (dpeaa)DE-He213 Lazkoz, Ruth verfasserin aut Sáez-Gómez, Diego verfasserin aut Salzano, Vincenzo verfasserin aut Enthalten in The European physical journal Berlin : Springer, 1998 76(2016), 11 vom: 19. Nov. (DE-627)253722934 (DE-600)1459069-4 1434-6052 nnns volume:76 year:2016 number:11 day:19 month:11 https://dx.doi.org/10.1140/epjc/s10052-016-4470-5 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2031 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2061 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2113 GBV_ILN_2119 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 33.50 ASE AR 76 2016 11 19 11
allfieldsSound	10.1140/epjc/s10052-016-4470-5 doi (DE-627)SPR008348944 (SPR)s10052-016-4470-5-e DE-627 ger DE-627 rakwb eng 530 ASE 33.50 bkl Beltrán Jiménez, Jose verfasserin aut Observational constraints on cosmological future singularities 2016 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In this work we consider a family of cosmological models featuring future singularities. This type of cosmological evolution is typical of dark energy models with an equation of state violating some of the standard energy conditions (e.g. the null energy condition). Such a kind of behavior, widely studied in the literature, may arise in cosmologies with phantom fields, theories of modified gravity or models with interacting dark matter/dark energy. We briefly review the physical consequences of these cosmological evolution regarding geodesic completeness and the divergence of tidal forces in order to emphasize under which circumstances the singularities in some cosmological quantities correspond to actual singular spacetimes. We then introduce several phenomenological parameterizations of the Hubble expansion rate to model different singularities existing in the literature and use SN Ia, BAO and H(z) data to constrain how far in the future the singularity needs to be (under some reasonable assumptions on the behavior of the Hubble factor). We show that, for our family of parameterizations, the lower bound for the singularity time cannot be smaller than about 1.2 times the age of the universe, what roughly speaking means %${\sim }2.8%$ Gyrs from the present time. Dark Energy (dpeaa)DE-He213 Dark Energy Model (dpeaa)DE-He213 Effective Field Theory (dpeaa)DE-He213 Null Energy Condition (dpeaa)DE-He213 Future Singularity (dpeaa)DE-He213 Lazkoz, Ruth verfasserin aut Sáez-Gómez, Diego verfasserin aut Salzano, Vincenzo verfasserin aut Enthalten in The European physical journal Berlin : Springer, 1998 76(2016), 11 vom: 19. Nov. (DE-627)253722934 (DE-600)1459069-4 1434-6052 nnns volume:76 year:2016 number:11 day:19 month:11 https://dx.doi.org/10.1140/epjc/s10052-016-4470-5 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2031 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2061 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2113 GBV_ILN_2119 GBV_ILN_2190 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 33.50 ASE AR 76 2016 11 19 11
language	English
source	Enthalten in The European physical journal 76(2016), 11 vom: 19. Nov. volume:76 year:2016 number:11 day:19 month:11
sourceStr	Enthalten in The European physical journal 76(2016), 11 vom: 19. Nov. volume:76 year:2016 number:11 day:19 month:11
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Dark Energy Dark Energy Model Effective Field Theory Null Energy Condition Future Singularity
dewey-raw	530
isfreeaccess_bool	true
container_title	The European physical journal
authorswithroles_txt_mv	Beltrán Jiménez, Jose @@aut@@ Lazkoz, Ruth @@aut@@ Sáez-Gómez, Diego @@aut@@ Salzano, Vincenzo @@aut@@
publishDateDaySort_date	2016-11-19T00:00:00Z
hierarchy_top_id	253722934
dewey-sort	3530
id	SPR008348944
language_de	englisch
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author	Beltrán Jiménez, Jose
spellingShingle	Beltrán Jiménez, Jose ddc 530 bkl 33.50 misc Dark Energy misc Dark Energy Model misc Effective Field Theory misc Null Energy Condition misc Future Singularity Observational constraints on cosmological future singularities
authorStr	Beltrán Jiménez, Jose
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topic_title	530 ASE 33.50 bkl Observational constraints on cosmological future singularities Dark Energy (dpeaa)DE-He213 Dark Energy Model (dpeaa)DE-He213 Effective Field Theory (dpeaa)DE-He213 Null Energy Condition (dpeaa)DE-He213 Future Singularity (dpeaa)DE-He213
topic	ddc 530 bkl 33.50 misc Dark Energy misc Dark Energy Model misc Effective Field Theory misc Null Energy Condition misc Future Singularity
topic_unstemmed	ddc 530 bkl 33.50 misc Dark Energy misc Dark Energy Model misc Effective Field Theory misc Null Energy Condition misc Future Singularity
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title	Observational constraints on cosmological future singularities
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title_full	Observational constraints on cosmological future singularities
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title_sort	observational constraints on cosmological future singularities
title_auth	Observational constraints on cosmological future singularities
abstract	Abstract In this work we consider a family of cosmological models featuring future singularities. This type of cosmological evolution is typical of dark energy models with an equation of state violating some of the standard energy conditions (e.g. the null energy condition). Such a kind of behavior, widely studied in the literature, may arise in cosmologies with phantom fields, theories of modified gravity or models with interacting dark matter/dark energy. We briefly review the physical consequences of these cosmological evolution regarding geodesic completeness and the divergence of tidal forces in order to emphasize under which circumstances the singularities in some cosmological quantities correspond to actual singular spacetimes. We then introduce several phenomenological parameterizations of the Hubble expansion rate to model different singularities existing in the literature and use SN Ia, BAO and H(z) data to constrain how far in the future the singularity needs to be (under some reasonable assumptions on the behavior of the Hubble factor). We show that, for our family of parameterizations, the lower bound for the singularity time cannot be smaller than about 1.2 times the age of the universe, what roughly speaking means %${\sim }2.8%$ Gyrs from the present time.
abstractGer	Abstract In this work we consider a family of cosmological models featuring future singularities. This type of cosmological evolution is typical of dark energy models with an equation of state violating some of the standard energy conditions (e.g. the null energy condition). Such a kind of behavior, widely studied in the literature, may arise in cosmologies with phantom fields, theories of modified gravity or models with interacting dark matter/dark energy. We briefly review the physical consequences of these cosmological evolution regarding geodesic completeness and the divergence of tidal forces in order to emphasize under which circumstances the singularities in some cosmological quantities correspond to actual singular spacetimes. We then introduce several phenomenological parameterizations of the Hubble expansion rate to model different singularities existing in the literature and use SN Ia, BAO and H(z) data to constrain how far in the future the singularity needs to be (under some reasonable assumptions on the behavior of the Hubble factor). We show that, for our family of parameterizations, the lower bound for the singularity time cannot be smaller than about 1.2 times the age of the universe, what roughly speaking means %${\sim }2.8%$ Gyrs from the present time.
abstract_unstemmed	Abstract In this work we consider a family of cosmological models featuring future singularities. This type of cosmological evolution is typical of dark energy models with an equation of state violating some of the standard energy conditions (e.g. the null energy condition). Such a kind of behavior, widely studied in the literature, may arise in cosmologies with phantom fields, theories of modified gravity or models with interacting dark matter/dark energy. We briefly review the physical consequences of these cosmological evolution regarding geodesic completeness and the divergence of tidal forces in order to emphasize under which circumstances the singularities in some cosmological quantities correspond to actual singular spacetimes. We then introduce several phenomenological parameterizations of the Hubble expansion rate to model different singularities existing in the literature and use SN Ia, BAO and H(z) data to constrain how far in the future the singularity needs to be (under some reasonable assumptions on the behavior of the Hubble factor). We show that, for our family of parameterizations, the lower bound for the singularity time cannot be smaller than about 1.2 times the age of the universe, what roughly speaking means %${\sim }2.8%$ Gyrs from the present time.
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title_short	Observational constraints on cosmological future singularities
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