source
stringlengths 1
2.05k
⌀ | target
stringlengths 1
11.7k
|
|---|---|
This grid was taken from ?.. | This grid was taken from \citet{Ryanetal1996a}. . |
Lf the intrinsic ellipticities of the galaxies are cross-correlated with the surrounding laree-seale density ield. then it will in turn lead to a cross-correlation between he gravitational lensing shear and the galaxy. ellipticities. | If the intrinsic ellipticities of the galaxies are cross-correlated with the surrounding large-scale density field, then it will in turn lead to a cross-correlation between the gravitational lensing shear and the galaxy ellipticities. |
tecent observations indeed. have reported: detections of he Gl correlation signals in low-redshift e&alaxv surveys (Alanclelbaumetal.2006:Hirata2007). | Recent observations indeed have reported detections of the GI correlation signals in low-redshift galaxy surveys \citep{man-etal06,hir-etal07}. |
.. To assess a »ossible systematic contamination of weak lensing due to the GL cross-corrclations. it will be important first to examine he relation between the observed GL cross-correlations and he ED cross-correlations of the cosmic web. | To assess a possible systematic contamination of weak lensing due to the GI cross-correlations, it will be important first to examine the relation between the observed GI cross-correlations and the ED cross-correlations of the cosmic web. |
This work will require incorporating a model for how the galaxy shapes are aligned relative to the dark matter (Llevmansetal.2006). | This work will require incorporating a model for how the galaxy shapes are aligned relative to the dark matter \citep{hey-etal06}. |
. Our future work is in this direction. | Our future work is in this direction. |
The Millennium Simulation analvzed. in this paper was carried out by the Vireo Supercomputing Consortium at the Computing Center of the Max-Planck Society in Garching. Germany. | The Millennium Simulation analyzed in this paper was carried out by the Virgo Supercomputing Consortium at the Computing Center of the Max-Planck Society in Garching, Germany. |
The simulation databases and the web application providing online access to them were constructed. as. part of the activities of the German Astrophysical Virtua Observatory. | The simulation databases and the web application providing online access to them were constructed as part of the activities of the German Astrophysical Virtual Observatory. |
G.L. works for the Cerman Astrophysica Virtual Observatory (CLAVOJwhich. is. supported by a erant from the German Federal Ministry of Eclucation anc Research (BAIBF) uncer contract 05 ACGVILA. | G.L. works for the German Astrophysical Virtual Observatory (GAVO),which is supported by a grant from the German Federal Ministry of Education and Research (BMBF) under contract 05 AC6VHA. |
We thank an anonymous referee for his/her constructive report which helped us improve significantly the origina manuscript. | We thank an anonymous referee for his/her constructive report which helped us improve significantly the original manuscript. |
We also thank S.DAL White for stimulating discussion. ancl useful suggestions. | We also thank S.D.M. White for stimulating discussion and useful suggestions. |
JL. is very gratefu to the warm. hospitality of the Max. Planck Institute. for Astrophysics (AIPA) in Garching where this work was initiated and performed. | J.L. is very grateful to the warm hospitality of the Max Planck Institute for Astrophysics (MPA) in Garching where this work was initiated and performed. |
J.L. acknowledges financial support from Ixorea Science and Engineering Foundation (IXOSELE) erant funded by the Ixorean Government (OST. NO. ROI- | J.L. acknowledges financial support from Korea Science and Engineering Foundation (KOSEF) grant funded by the Korean Government (MOST, NO. R01-2007-000-10246-0). |
of the object. but the presence of even a weak AGN in Arp 220 would support a connection between ULIRGs and quasars (Sanders οἱ al. | of the object, but the presence of even a weak AGN in Arp 220 would support a connection between ULIRGs and quasars (Sanders et al. |
1983). | 1988). |
Wit is not an AGN. we cannot rule out the presence of a true AGN behind a Compton screen of column e10em 7. | If it is not an AGN, we cannot rule out the presence of a true AGN behind a Compton screen of column $\sim10^{25}\mbox{cm$ $}$. |
IE XRBs are responsible for the emission then a large number of conventional NlDs are needed. or a smaller number of ultraluminous ULX sources. | If XRBs are responsible for the emission then a large number of conventional XRBs are needed, or a smaller number of ultraluminous ULX sources. |
Ii either case. the concentration of these objects in the very centre of Arp 220 might indicate that these objects will later merge together to form a supermassive black hole and AGN (Taniguehi et al. | In either case, the concentration of these objects in the very centre of Arp 220 might indicate that these objects will later merge together to form a supermassive black hole and AGN (Taniguchi et al. |
1999). | 1999). |
Η there is a weak ACN already in the nuclear regions. then this process may already have begun. | If there is a weak AGN already in the nuclear regions, then this process may already have begun. |
We acknowledge use of the ADS. NED. and CLAO. | We acknowledge use of the ADS, NED, and CIAO. |
Partial support [or Chis work was provided bv the National Aeronautics and Space Acministration through Chandra Award Niunber GOI-1166 issued by the Chandra. X-Ray Observatory Center. which is operated bv the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-39073. | Partial support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO1-1166 issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-39073. |
S. Lamb acknowledges support from the DOE. through LLNL. | S. Lamb acknowledges support from the DOE, through LLNL. |
DLC and ACD were supported by PPARC. CM by the Roval Society. | DLC and ACB were supported by PPARC, CM by the Royal Society. |
We would also like to acknowledge the contributions of Bernie Peek and Charlie Baker to this work. | We would also like to acknowledge the contributions of Bernie Peek and Charlie Baker to this work. |
inwards. and couple with outgoing sound waves at the inner boundary of the postshock accretion [low. | inwards, and couple with outgoing sound waves at the inner boundary of the postshock accretion flow. |
Upon reaching the outer shock. (hese sound waves further distort the shock front. leading to a positive feedback. | Upon reaching the outer shock, these sound waves further distort the shock front, leading to a positive feedback. |
While (he mechanisms of Blondin&Mezzacappa and Foglizzo(2002) appear to produce similar outcomes in non-rotating cases. indeed Foelizzoetal.(2007) actually confirm the numerical values of [frequencies ancl growth rates measured by Dlondin&Alezzacappa(2006).. il is possible the presence of rotation might lead to substantial differences. which we discuss further below. | While the mechanisms of \citet{blondin05} and \citet{foglizzo02} appear to produce similar outcomes in non-rotating cases, indeed \citet{foglizzo06} actually confirm the numerical values of frequencies and growth rates measured by \citet{blondin05}, it is possible the presence of rotation might lead to substantial differences, which we discuss further below. |
Instabilies of the accretion shock also are observed in simulations will a more accurate treatment of supernova microplhvsies. with a realistic equation of state. neutrino (iransport and attendant nuclear reactions. ancl more physically motivated boundary conditions. | Instabilities of the accretion shock also are observed in simulations with a more accurate treatment of supernova microphysics, with a realistic equation of state, neutrino transport and attendant nuclear reactions, and more physically motivated boundary conditions. |
Schecketal.(2004) and Scheckοἱal.(2006) investigate the role of such instabilities in generating pulsar natal kicks. while Ixifonidisetal.(2005) study the ejection of metal clunps to the outer reeions of supernova ejecta. | \citet{scheck04} and \citet{scheck06} investigate the role of such instabilities in generating pulsar natal kicks, while \citet{kifonidis05}
study the ejection of metal clumps to the outer regions of supernova ejecta. |
Burrowsetal.(2006) also see the standing accretion shock instability 100 - 300 ms postbounce. | \citet{burrows05} also see the standing accretion shock instability 100 - 300 ms postbounce. |
The important feature of their simulation. though. is a core eravily wave al late times thal transfers acoustic power to the shock to continue powering the explosion. the initial perturbation for which is possibly seeded by the accretion shock instability. | The important feature of their simulation, though, is a core gravity wave at late times that transfers acoustic power to the shock to continue powering the explosion, the initial perturbation for which is possibly seeded by the accretion shock instability. |
Burrowsetal.(2006) also favor the interpretation of ol an advective-acoustic evele. though in this and the other more realistic simulations cited above. the exact mechanism of instability is difficult to. identify. | \citet{burrows05} also favor the interpretation of \citet{foglizzo06} of an advective-acoustic cycle, though in this and the other more realistic simulations cited above, the exact mechanism of instability is difficult to identify. |
To avoid this problem. Ohnishi.Ikotalke&Yaanada(2006) performed numerical simulations based on unperturbed spherically symmetrical shock accretion [lows given by Yamasaki&Yamada(2005)... a sort of middle ground” between (he acliabatic (lows of Dlondin.Mezzacappa&DeMarino(2003) and Bloudin&Mezzacappa(2006) aud the full supernova sinnuationus of other workers. | To avoid this problem, \citet{ohnishi05} performed numerical simulations based on unperturbed spherically symmetrical shock accretion flows given by \citet{yamasaki05}, a sort of “middle ground” between the adiabatic flows of \citet{blondin03} and \citet{blondin05} and the full supernova simulations of other workers. |
Ohnishi.IXotake&Yamada.(2006) clearly icentify ancl measure growth rates for /=1 and 2 mode instabilities. | \citet{ohnishi05} clearly identify and measure growth rates for $l=1$ and 2 mode instabilities. |
The real parts of the Irequencies scale with m(l/e;+t1fo)dr. the integral between the inner radius of the accretion flow and the shock of the sum of (he inverses of the sound speed ancl aclvection speed. suggesting (hat an advective-acoustic mechanism. as advanced by Foglizzo(2002) and Foglizzoetal.(2007).. is at work. | The real parts of the frequencies scale with $\int _{r_i}^{r_s}\left(1/c_s +1/v_r\right) dr$, the integral between the inner radius of the accretion flow and the shock of the sum of the inverses of the sound speed and advection speed, suggesting that an advective-acoustic mechanism, as advanced by \citet{foglizzo02} and \citet{foglizzo06}, is at work. |
However Ohnishi.lxotake&Yamacla(2006) only perturb the radial velocity component of the initially spherical symmetrical unperturbed flow. which may unduly influence their results. compared to allowing perturbations in polar and azimuthal directions as well. | However \citet{ohnishi05} only perturb the radial velocity component of the initially spherical symmetrical unperturbed flow, which may unduly influence their results, compared to allowing perturbations in polar and azimuthal directions as well. |
Yamasaki(2006) include rather more physies. aud again based on the [frequencies at which modes grow. conclude that an advective-acoustic cvele is al work. | \citet{yamasaki06} include rather more physics, and again based on the frequencies at which modes grow, conclude that an advective-acoustic cycle is at work. |
In (his work we present another approach to the problem. | In this work we present another approach to the problem. |
Following the work of on planar shocks in the interstellar medium. we derive an approximate dispersion relation lor oscillations of (he accretion shock by adding the effect of a gravitational [ield and spherical geometry. | Following the work of \citet{vishniac89} on planar shocks in the interstellar medium, we derive an approximate dispersion relation for oscillations of the accretion shock by adding the effect of a gravitational field and spherical geometry. |
In the case that the postshock advection is neglected. a quartic | In the case that the postshock advection is neglected, a quartic |
the more gradual build up of planetesimals to form a rocky core followed by accretion of gaseous material (Pollacketal.1996). | the more gradual build up of planetesimals to form a rocky core followed by accretion of gaseous material \citep{Pollack96}. |
. In both class of models. the accretion disk Lifetime sets au important time scale ou the planet formation process by constraiuiug the time available for a gravitational instability to develop or the rocky core to form before the gas aud dust are clissipatect. | In both class of models, the accretion disk lifetime sets an important time scale on the planet formation process by constraining the time available for a gravitational instability to develop or the rocky core to form before the gas and dust are dissipated. |
Circumstellar accretion disks around young stars are commonly inferred based ou the presence of iufrared emission in excess of the stellar photosphere. | Circumstellar accretion disks around young stars are commonly inferred based on the presence of infrared emission in excess of the stellar photosphere. |
In many stars the excess infrared emission from ccan be modeled with a geometrically thin. optically thick accretion disk. L).. although inner disk holes. flariug. aud other refinements to this basic model :we often ueecled to reproduce the observations iu detail (Adams.Shu.&Lada10988:Calvetetal.1991.92:&Goldreich 1997). | In many stars the excess infrared emission from can be modeled with a geometrically thin, optically thick accretion disk \citep{Lynden74}, although inner disk holes, flaring, and other refinements to this basic model are often needed to reproduce the observations in detail \citep{Adams88,Calvet91,Chiang97}. |
. Detailed spectral energy distributions Iron the near- to Car-intared have been compiled [or only a few nearby star forming reeious (e.g. Strom 1980:Wκας, Lada. Young 1989). but J-. H-. K-. and L-baud imaging studies yrovide au efficieut 1leaus (oO search for near-infrared) excesses iu. hundreds of stars (often in elusters) of va‘ious ages. | Detailed spectral energy distributions from the near- to far-infrared have been compiled for only a few nearby star forming regions (e.g. Strom 1989;Wilking, Lada, Young 1989), but $J$ -, $H$ -, $K$ -, and $L$ -band imaging studies provide an efficient means to search for near-infrared excesses in hundreds of stars (often in clusters) of various ages. |
Recent results iudicate that at least of solar mass stars at an age of | Myr exhijt a near-infrared excess. but that the percentage decreases to for ages 3-10 Myr (Strom&Lada 2001b). | Recent results indicate that at least of solar mass stars at an age of 1 Myr exhibit a near-infrared excess, but that the percentage decreases to for ages 3-10 Myr \citep{Strom89,Haisch01b}. |
. These results are consistent. with the iotion that the ifetime of accretion disks around most solar mass stars is 3-10 Myr. | These results are consistent with the notion that the lifetime of accretion disks around most solar mass stars is 3-10 Myr. |
Strictly speaking. a near-iufrared. excess is cliaguosic of only hot «ust with temperatures of 1000 Ix. For a solar nass star. these temperatures are found only. within 0.1 AU of the star. | Strictly speaking, a near-infrared excess is diagnostic of only hot dust with temperatures of 1000 K. For a solar mass star, these temperatures are found only within 0.1 AU of the star. |
Most of the dust mass. aud presumably the majority of glanet formation. will be located at larger racii aud have temperatures too cool to raciate in the nea-jufrared. | Most of the dust mass, and presumably the majority of planet formation, will be located at larger radii and have temperatures too cool to radiate in the near-infrared. |
Further. some disks are thought to have inner holes such that stars without near-infrared excesses iuay still contain substautial disk masses. ( | Further, some disks are thought to have inner holes such that stars without near-infrared excesses may still contain substantial disk masses. ( |
Although observatiois suggest that the transition [from an optically tlick to au optically thin disk occurs ou time scales of 0.3 Myr. tu which case near-iufrared observatiOLS thay in fact provide an iudirect probe of the larger scale disk: Skrutskie 1990. see also Haisch. Lada. Lada 2001a). | Although observations suggest that the transition from an optically thick to an optically thin disk occurs on time scales of 0.3 Myr, in which case near-infrared observations may in fact provide an indirect probe of the larger scale disk; Skrutskie 1990, see also Haisch, Lada, Lada 2001a). |
An additional limitation of near-infrared studies is that the emissiol is optically thick and. provides little ineaniugful coustraiuts ou the disk mass (see. e.g.. Woo 2002). | An additional limitation of near-infrared studies is that the emission is optically thick and provides little meaningful constraints on the disk mass (see, e.g., Wood 2002). |
Longer wavelength observations are needed to establish tle disk lifetime at large oral radii aud to provide measures ou how disk masses evolve with time. | Longer wavelength observations are needed to establish the disk lifetime at large orbital radii and to provide measures on how disk masses evolve with time. |
Millimeter aud submillimeter corμαι emission are tle best avaiable tracers of dust in the cool. outer disk. | Millimeter and submillimeter continuum emission are the best available tracers of dust in the cool, outer disk. |
The most compreheusive continuum surveys to date lias'e been toward voung stars in Taurus (Beckwithetal.1090:Osteroh&Beckwith1995:MotteAixré2001).. p Oph Nlontiuerle199£:Nürnbergeretal.1998:Motte.André.&Neri 1998).. Ltpus (Nürnberger.Clini.&Zinnecker 1997).. Chamaeleou I (Heningοἱal.1903).. aud Serpeus (Testi&Sargent 1993).. | The most comprehensive continuum surveys to date have been toward young stars in Taurus \citep{Beckwith90,OB95,Motte01}, $\rho$ Oph \citep{Andre94,N98,Motte98}, Lupus \citep{N97}, Chamaeleon I \citep{Henning93}, and Serpens \citep{Testi98}. . |
These observations have 5lown that at zu age of 1 Myr. of the stars possess a circumstellar cisk | These observations have shown that at an age of 1 Myr, of the stars possess a circumstellar disk |
N-body ¢odes are one of the most important tools of theoretical cosinology because they offer the possiylity of simulating most of the gravitational processes driving the formation of the large scale structure of the universe (hereafter LSS} Ἐ | N-body codes are one of the most important tools of theoretical cosmology because they offer the possibility of simulating most of the gravitational processes driving the formation of the large scale structure of the universe (hereafter LSS) . |
ν, These simulations are often used to check cosmological | These simulations are often used to check cosmological |
dillieult to detect. but might have the serendipitous fortune of resolving the cooling Low problem (Fabianctal.1994). | difficult to detect, but might have the serendipitous fortune of resolving the cooling flow problem \citealt{fabian94}) ). |
Unfortunately. even if the cluster dark matter problem were resolved. there remains the issue of cosmological dark matter. | Unfortunately, even if the cluster dark matter problem were resolved, there remains the issue of cosmological dark matter. |
Put simply. there is compelling evidence that the Universe consists of a form of dark. energy. (like a cosmological constant) that forces the expansion of the Universe to accelerate at late times (Perlmutteretal.1999:Schmidtetal. 1998)). | Put simply, there is compelling evidence that the Universe consists of a form of dark energy (like a cosmological constant) that forces the expansion of the Universe to accelerate at late times \citealt{perlmutter99,schmidt98}) ). |
However. we have no idea what this dark energy is (Dialerio 2008)) from a particle physics point of view. although perhaps thecoincidence between e, and ell, or ολΑΣ is a strong indication. (Milerom.2002. 2008)). | However, we have no idea what this dark energy is \citealt{diaferio08a}) ) from a particle physics point of view, although perhaps thecoincidence between $a_o$ and $cH_o$ or $c(\Lambda/3)^{1/2}$ is a strong indication \citealt{milgrom02,milgrom08}) ). |
With the presence of this dark energy. in order. for the Universe not to expand too rapidly. there needs to be some form of matter independent of the well fixed. quantity of barvons to endow the Universe with additional inertia. | With the presence of this dark energy, in order for the Universe not to expand too rapidly, there needs to be some form of matter independent of the well fixed quantity of baryons to endow the Universe with additional inertia. |
This additional matter serves several purposes: it allows for large structures to form more rapidly out of the expanding Universe which is shown by the matter power spectrum at large scales Clegmarketal. 2004)). | This additional matter serves several purposes: it allows for large structures to form more rapidly out of the expanding Universe which is shown by the matter power spectrum at large scales \citealt{tegmark04}) ). |
Also. it drives the collapse of the photon-barvyon [uid to form fluctuations in the cosmic microwave background (CM) at well measured angular scales (Whiteetal. 1994)) and it gives the correct distance-redshift relation (expansion history). | Also, it drives the collapse of the photon-baryon fluid to form fluctuations in the cosmic microwave background (CMB) at well measured angular scales \citealt{white94}) ) and it gives the correct distance-redshift relation (expansion history). |
The underlving theory of MOND is still unknown. also it is only a classical framework. so a huge elfort was mace to extend MOND to the relativistic regime. | The underlying theory of MOND is still unknown, also it is only a classical framework, so a huge effort was made to extend MOND to the relativistic regime. |
In 2004. a giant leap was mace in this direction by Bekenstein(2004) and others have taken to thrashing out the predictions of other AIOND inspired relativistic theories (Sanders2005:Sko-τοιςetal.2006:Zlosnik2006. 2007a.b)). | In 2004, a giant leap was made in this direction by \cite{bekenstein04} and others have taken to thrashing out the predictions of other MOND inspired relativistic theories \citealt{sanders05,skordis06,zlosnik06,zlosnik07a,zlosnik07b}) ). |
Sadlv. the predictions for cosmology are not clear and. there seenis to be too much freedom. in contradiction to the absolute predictiveness of MOND in galaxies. | Sadly, the predictions for cosmology are not clear and there seems to be too much freedom, in contradiction to the absolute predictiveness of MOND in galaxies. |
For this reason. E show here the predictions of coupling MOND with sterile neutrino dark matter using the employed. by MeGaugh(2004) when matching the CAIB with MOND ie. that no MOND ellects are. present before recombination. | For this reason, I show here the predictions of coupling MOND with sterile neutrino dark matter using the employed by \cite{mcgaugh04} when matching the CMB with MOND i.e. that no MOND effects are present before recombination. |
A simple argument supporting this is that at a redshift of ς —1080 the angular diameter clistance to recombination 24=l4Cpe and the angular scale. 8. of the first (ancl largest) peak is 1" or 0.01Trad. | A simple argument supporting this is that at a redshift of $z\sim$ 1080 the angular diameter distance to recombination $D_A=14Gpc$ and the angular scale, $\theta$ , of the first (and largest) peak is $1^o$ or 0.017rad. |
So the physical size of the first peak r=06D is ~240\Mpe. | So the physical size of the first peak $r=\theta D_A$ is $\sim$ 240Mpc. |
Since the average overdensity ὁ is only 1. parti in 107 of the critical density pe(2). the tvpical eravities at a radius r from the centre of one of these overdensities is g=GdAL(r)r7158p,(z)r where pols)= and HG=MIO,|dOs. | Since the average overdensity $\delta$ is only $1$ part in $10^5$ of the critical density $\rho_c(z)$, the typical gravities at a radius $r$ from the centre of one of these overdensities is $g=G\delta M(r)r^{-2}={4\pi \over 3} G\delta\rho_c(z)r$ where $\rho_c(z)={3H(z)^2 \over 8\pi G}$ and $H(z)^2=H_o^2[\Omega_m(1+z)^3 +\Omega_{\Lambda}$. |
Compiling all this HSgives iH. right] AM or=2404pe. where aq,=3.6(kmstype5 ds the MOND acceleration constant. | Compiling all this gives H_o^2 ]r At $r=240Mpc$, where $a_o=3.6(\kms)^2pc^{-1}$ is the MOND acceleration constant. |
Typical accelerations so many. times ereater than αρ are completely unalfected by NIOND gravity and therefore no MOND elfects should influence the ςMD. | Typical accelerations so many times greater than $a_o$ are completely unaffected by MOND gravity and therefore no MOND effects should influence the CMB. |
Llowever. as 2 drops. so does p(s) and thus peculiar accelerations can slide into the MOND regime. | However, as $z$ drops, so does $\rho_c(z)$ and thus peculiar accelerations can slide into the MOND regime. |
Thus. the matter power spectrum can be allected by MOND. | Thus, the matter power spectrum can be affected by MOND. |
Lt is often forgotten when looking at MOND cosmology that cold dark matter exists in MOND. | It is often forgotten when looking at MOND cosmology that cold dark matter exists in MOND. |
Therefore. we must relax many of the constraints that are set by CDM cosmology. | Therefore, we must relax many of the constraints that are set by CDM cosmology. |
“The most important. ancl obvious one is that there is now a large gap in the energv-density budget since CDAL is not present and it is perfectly. reasonable to fill this eap with hot dark matter like neutrinos. | The most important and obvious one is that there is now a large gap in the energy-density budget since CDM is not present and it is perfectly reasonable to fill this gap with hot dark matter like neutrinos. |
Phe constraints on neutrino masses. for which cosmology is still the most stringent. must be reanalysecl in light of MOND. | The constraints on neutrino masses, for which cosmology is still the most stringent, must be reanalysed in light of MOND. |
Still. the empirical evidence from supernovae data (Schmidtotal.1998:Perlmutteretal. 1999)) strongly suggest the universes expansion is accelerating owed to the existence. of dark energv. Oy. | Still, the empirical evidence from supernovae data \citealt{schmidt98,perlmutter99}) ) strongly suggest the universes expansion is accelerating owed to the existence of dark energy, $\Omega_{\Lambda}$. |
Furthermore. the barvon. budget is. strongly constrained by well understood physics to be around 0,47~(0.015—0.025 (Bocsgaarcd&Steigman1985:Burlesetal.2001:MeCGaugh 2004)). but this still leaves a large amount of latitucle in the energy budget for DM. | Furthermore, the baryon budget is strongly constrained by well understood physics to be around $\Omega_bh^2\sim 0.015-0.025$ \citealt{boesgaard85,burles01,mcgaugh04}) ), but this still leaves a large amount of latitude in the energy budget for DM. |
Any DAL however. must. be compatable with clusters of galaxies. the well understood lack of DAL in galaxies in MOND and the anisotropies in the angular power spectrum of the CAIB. | Any DM, however, must be compatable with clusters of galaxies, the well understood lack of DM in galaxies in MOND and the anisotropies in the angular power spectrum of the CMB. |
Phe best candidates for such hot DAL are neutrinos. | The best candidates for such hot DM are neutrinos. |
The three active neutrinos (7j. 9A and 9.) from the standard model of particle physics have been shown to mix between Iavours by atmospheric and. solar neutrino experiments (Ahmadetal.2001:Ashie 2004)). | The three active neutrinos $\nu_{\mu}$, $\nu_{e}$ and $\nu_{\tau}$ ) from the standard model of particle physics have been shown to mix between flavours by atmospheric and solar neutrino experiments \citealt{ahmad01,ashie04}) ). |
However. the exact masses of the three active neutrinos are not vet known. only their squared mass dilferences. | However, the exact masses of the three active neutrinos are not yet known, only their squared mass differences. |
Nevertheless. the masses of all three are known to be less than 2.2eV. [rom the Mainz-‘Troitz experiments (Ixrausetal. 2005)). | Nevertheless, the masses of all three are known to be less than 2.2eV from the Mainz-Troitz experiments \citealt{kraus05}) ). |
The maximum censity that a neutrino species can produce after gravitational collapse is given by the limit (CIremaine&Gunn 1979)). yl for each of the three species. | The maximum density that a neutrino species can produce after gravitational collapse is given by the Tremain-Gunn limit \citealt{tremaine79}) ), )^4 for each of the three species. |
Thus. the density is greatly dependent on the mass of the neutrinos. | Thus, the density is greatly dependent on the mass of the neutrinos. |
However. groups and clusters of galaxies have dark matter that is much denser than can be produced. by the active neutrinos even at the maximum mass of 2.2cV (Angusctal. 2008)). | However, groups and clusters of galaxies have dark matter that is much denser than can be produced by the active neutrinos even at the maximum mass of 2.2eV \citealt{afb}) ). |
H£ the dark matter is indeed a neutrino like species. it must be heavier than SeV. (Aneusetal. 2008)). | If the dark matter is indeed a neutrino like species, it must be heavier than 8eV \citealt{afb}) ). |
Phere is a further problem. with neutrinos at 2.20V in that the contribution they make to the energy density of the Universe is given by —00205m,.. meaning that at 2.20V thethree neutrinos make a contribution to the energy density of the Universe. but the nmiaximum cdensity is relatively low (see Eq 2)). | There is a further problem with neutrinos at 2.2eV in that the contribution they make to the energy density of the Universe is given by , meaning that at 2.2eV thethree neutrinos make a contribution to the energy density of the Universe, but the maximum density is relatively low (see Eq \ref{eqn:tg}) ). |
Such a huge contribution would be easily detectable in the angular power spectrum of the fluctuations in the CMD as shown for this | Such a huge contribution would be easily detectable in the angular power spectrum of the fluctuations in the CMB as shown for this |
behavior. | behavior. |
For the other classes, the shows behavior similar to a non-linear chaotic system systemwith some inherent stochastic noise. | For the other classes, the system shows behavior similar to a non-linear chaotic system with some inherent stochastic noise. |
Before considering the implications, it is prudent to emphasize that the results presented here need to be confirmed more comprehensive non-linear data analysis. | Before considering the implications, it is prudent to emphasize that the results presented here need to be confirmed by more comprehensive non-linear data analysis. |
Since the resultsby are based on a null hypothesis test involving surrogate data, a more comprehensive test should take into account possible different kinds of surrogate data. | Since the results are based on a null hypothesis test involving surrogate data, a more comprehensive test should take into account possible different kinds of surrogate data. |
because of the effects of phase averaging aud redshifts on the observed spectra. | because of the effects of phase averaging and redshifts on the observed spectra. |
In this paper. we have considered the various effects of vacuum polarization aud proton cyclotron resonances ou the propagation of photous tl‘ough a stronely inaguetized plasma. | In this paper, we have considered the various effects of vacuum polarization and proton cyclotron resonances on the propagation of photons through a strongly magnetized plasma. |
Subsets and Splits
No community queries yet
The top public SQL queries from the community will appear here once available.