ReadingTimeMachine/rtm-sgt-ocr-v1 · Datasets at Hugging Face

Mass loss accompanying stellar evolution moclilies the picture. but does uot change it qualitatively.

Mass loss accompanying stellar evolution modifies the picture, but does not change it qualitatively.

Siuce the most massive stars die out belore they cau couple with others. the degree of binary heating. aud therefore the vigor of global expausion. is less.

Since the most massive stars die out before they can couple with others, the degree of binary heating, and therefore the vigor of global expansion, is less.

Iu addition. the earlier phase of core contraction lasts longerOm aud leads to a higherfae) central density before reversal.

In addition, the earlier phase of core contraction lasts longer and leads to a higher central density before reversal.

Both moclificatious iucrease with the cluster population NV.

Both modifications increase with the cluster population $N$.

We thus see why some globular clusters iudeed reach the point of true core collapse. which cau be reversed ouly by the tightest of binaries.

We thus see why some globular clusters indeed reach the point of true core collapse, which can be reversed only by the tightest of binaries.

The new picture of cluster evolution preseuted here is more complex than tle classical oue. but it is motivated by the basic physical effects that are incorporated in moderni uumerical simulatious.

The new picture of cluster evolution presented here is more complex than the classical one, but it is motivated by the basic physical effects that are incorporated in modern numerical simulations.

With the beneli X hiudsight. i is easy to see why earlier. simplified methods reinforced the impression that cyuamical relaxation is ubiquitous.

With the benefit of hindsight, it is easy to see why earlier, simplified methods reinforced the impression that dynamical relaxation is ubiquitous.

Iu sinele mass mocels. binary formation is so delayed that it becomes irrelevant.

In single mass models, binary formation is so delayed that it becomes irrelevant.

Statistical models. based ou solving the Fokker-Plauck equation. ieglect three-bocly effects eutirely.

Statistical models, based on solving the Fokker-Planck equation, neglect three-body effects entirely.

—- Finally. the contraction of Lagrangian nass shells is not a reliable sien of core contraction. but may reflect a differeut phenomenon. mass segregation.

Finally, the contraction of Lagrangian mass shells is not a reliable sign of core contraction, but may reflect a different phenomenon, mass segregation.

Our uew picture is itself far [roin complete.

Our new picture is itself far from complete.

Future simulations carried out at higher JN. will reveal iu detail how the ransition is mace to a more vigorously contractiug central core.

Future simulations carried out at higher $N$ will reveal in detail how the transition is made to a more vigorously contracting central core.

We are grateful to Douglas Hegegle and Simou Portegies-Zwart for hielpiug us navigate the literature of dynamical relaxation.

We are grateful to Douglas Heggie and Simon Portegies-Zwart for helping us navigate the literature of dynamical relaxation.

Ousi Fakhourt also provided useful suggestious ou the visualization of energy transfer.

Onsi Fakhouri also provided useful suggestions on the visualization of energy transfer.

This research was supported by NSF gerant. AST 0008573.

This research was supported by NSF grant AST 0908573.

ercater than those of NGC 7603 and its companion galaxy.

greater than those of NGC 7603 and its companion galaxy.

Thus we have preseuted a very well known svstenmi with anomalous redshifts. NCC 7603. to be an apparently much more anomalous than was previously thought.

Thus we have presented a very well known system with anomalous redshifts, NGC 7603, to be an apparently much more anomalous than was previously thought.

There are | objects with very different redshifts apparently commected by a filament associated with the lower redshift galaxy.

There are 4 objects with very different redshifts apparently connected by a filament associated with the lower redshift galaxy.

This svstem is at prescut the most spectacular case that we know among the caudidates for anomalous redshift.

This system is at present the most spectacular case that we know among the candidates for anomalous redshift.

Future studies of this system are clearly warranted.

Acknowledements: We eratefully acknowledge the anonviuous referee for helpful conunents.

Acknowledgments: We gratefully acknowledge the anonymous referee for helpful comments.

Thanks are also eivon to Victor P. Debattista aud Ciustav Tanunaun (Astron.

Thanks are also given to Victor P. Debattista and Gustav Tammann (Astron.

Inst.

Basel) for helpfu discussion about the present paper.

Basel) for helpful discussion about the present paper.

the remnant at the center.

A reduction in the infall mass brings z15D closer to reproducing observations.

Two dimensional versions of the one dimensional simulations presented in the higher energy explosions of 7 and ? might eject more of the pproduced in the more energetic explosions.

Two dimensional versions of the one dimensional simulations presented in the higher energy explosions of \citet{Heger&Woosley:2008} and \citet{Nomoto:2007} might eject more of the produced in the more energetic explosions.

Rotating models (7) create more primary nitrogen, which can lead to an increase in the rate of CNO burning at the base of the hydrogen shell, causing some models die as larger red supergiants rather than a compact blue supergiants.

Rotating models \citep{Hirschi:2008} create more primary nitrogen, which can lead to an increase in the rate of CNO burning at the base of the hydrogen shell, causing some models die as larger red supergiants rather than a compact blue supergiants.

In this case, Rayleigh-Taylor mixing would play out in a similar way to the solar models presented in this paper, and more iron would

In this case, Rayleigh-Taylor mixing would play out in a similar way to the solar models presented in this paper, and more iron would be ejected by these stars.

point out that the supernova explosion mechanism is probably inherently multidimensional and asymmetric.

Recent simulations \citep{Scheck:2004,Scheck:2006,Burrows:2007a,Burrows:2007b, Burrows:2007c} point out that the supernova explosion mechanism is probably inherently multidimensional and asymmetric.

Asymmetry in the explosion, whether in the form of a jet or a perturbation described by Legendre polynomials of order of |=1 or |=2, might also mix more of the nickel core out of the star, bringing the models closer to reproducing observations.

Asymmetry in the explosion, whether in the form of a jet or a perturbation described by Legendre polynomials of order of $l=1$ or $l=2$, might also mix more of the nickel core out of the star, bringing the models closer to reproducing observations.

7 have suggested that HMP stars may be "chemically peculiar" stars, in which low iron abundance is caused by separation of gas and dust beyond the stellar surface, followed by accretion of dust-depleted gas.

\citet{Venn&Lambert:2008} have suggested that HMP stars may be ”chemically peculiar” stars, in which low iron abundance is caused by separation of gas and dust beyond the stellar surface, followed by accretion of dust-depleted gas.

If this is the case-and the authors note that a definitive answer requires additional information—the stars’ true metallicity is closer to [X/H] z—2 rather than -5.

If this is the case–and the authors note that a definitive answer requires additional information--the stars' true metallicity is closer to [X/H] $\approx -2$ rather than -5.

'The supernova light curve is affected by the amount of 56ΝΙ in the center of the star that falls back onto the black hole at the center of the explosion.

The supernova light curve is affected by the amount of $^{56}$ Ni in the center of the star that falls back onto the black hole at the center of the explosion.

The models for the first supernovae presented in this work are intrinsically dimmer than corresponding supernovae arising from stars of solar composition provided they explode with the same amount of energy.

In our models of primordial composition supernovae, all or nearly all of the synthesized in the supernova falls back onto the remnant left behind at the center of the explosion.

Energy from the radioactive decay of powers the tail of core-collapse supernova light curves.

When the energy released in its radioactive decay to °°Fe is no longer observable, the supernova light curves will loose their radioactive tails, making them briefer and dimmer than ordinary core-collapse supernova light curves.

When the energy released in its radioactive decay to $^{56}$ Fe is no longer observable, the supernova light curves will loose their radioactive tails, making them briefer and dimmer than ordinary core-collapse supernova light curves.

The presupernova structure of a star is determined largely by its initial mass and by the initial composition of the gas from which it formed.

The symmetry and energy of the explosion, along with the presupernova structure, influence where and to what extent Rayleigh- instabilities will grow, as well as how much mass will fall back onto the remnant at the center.

The symmetry and energy of the explosion, along with the presupernova structure, influence where and to what extent Rayleigh-Taylor instabilities will grow, as well as how much mass will fall back onto the remnant at the center.

The non-rotating zero metallicity models studied are far more compact than solar-composition models of the same mass, in part because CNO burning proceeds at higher temperatures and densities.

CNO burning is responsible for energy production during the main sequence for all stars at the masses studied here, but in metal poor stars CNO burning proceeds at higher temperatures and densities.

For zero-metalicity stars, the star must first contract to a temperature of 10? K, hot enough to initiate helium burning.

For zero-metalicity stars, the star must first contract to a temperature of $^8$ K, hot enough to initiate helium burning.

This helium burning produces a small amount of carbon, which is enough to act as a catalyst to enable hot CNO burning to proceed.

In addition, non-rotating stars with a metallicity Z below 10-? will never reach the red giant branch, since they end helium burning with effective temperatures above 104.

In addition, non-rotating stars with a metallicity Z below $^{-3}$ will never reach the red giant branch, since they end helium burning with effective temperatures above $^4$.

Below this temperature, the opacity is large enough that the star will expand toward the red giant branch.

The more compact structure of these stars causes their reverse shocks to propagate more quickly to the origin than those in solar stars.

Larger remnants are left behind in the more compact stars because the rate at which mass accretes onto the stellar remnant is higher, as predicted by ? and shown in the 1D simulations of ?..

Larger remnants are left behind in the more compact stars because the rate at which mass accretes onto the stellar remnant is higher, as predicted by \citet{Chevalier:1989} and shown in the 1D simulations of \citet{Zhang:2008}.

The time scale over which the Rayleigh-Taylor instabilities can develop is also set by the reverse shock.

For the case of the compact primordial composition progenitors modeled here, the Rayleigh-Taylor instabilities have little time to develop.

This means that a smaller portion of the isotopic layers of the star will be mixed.

The Rayleigh-Taylor instabilities do not have time to become fully nonlinear in our simulations, so the scale of the instability as well as the degree of mixing is set by the scale of the initial seed perturbations.

In the case of the solar-composition progenitor models, the Rayleigh-Taylor instability became fully nonlinear and the size and shape of the initial perturbation was no longer apparent at late times.

A smaller region of the primordial-composition stars is unstable, compared to solar-composition stars, which also contributes to the reduced mixing we see in our zero-metal models.

The small amount of mixing

As the largest virtalized objects in. the Universe. galaxy clusters are a powerful cosmological tool once their mass distribution is univocally determined.

As the largest virialized objects in the Universe, galaxy clusters are a powerful cosmological tool once their mass distribution is univocally determined.

In the recent past. there have been several claims that cluster masses obtained from X-ray analyses of the intracluster plasma. taken to be in hydrostatic equilibrium with the gravitational potential well. are significantly smaller (up to a factor of two: but see Wu et 11998: Allen 1998; Bóhhringer et 1998; Allen et 22001) than the ones derived from gravitational lensing (see Mellier 1999 for a review).

In the recent past, there have been several claims that cluster masses obtained from X-ray analyses of the intracluster plasma, taken to be in hydrostatic equilibrium with the gravitational potential well, are significantly smaller (up to a factor of two; but see Wu et 1998; Allen 1998; Böhhringer et 1998; Allen et 2001) than the ones derived from gravitational lensing (see Mellier 1999 for a review).

In this paper we report on the mass distribution. of the cluster 1224 by combining the results from weak lensing analysis of deep FORSI-VLT images with those obtained from a spatially-resolved spectroscopic X-ray analysis of a observation.

In this paper we report on the mass distribution of the cluster $-$ 1224 by combining the results from weak lensing analysis of deep FORS1-VLT images with those obtained from a spatially-resolved spectroscopic X-ray analysis of a observation.

1224 is a rich galaxy cluster at redshift 0.302 that has been part of the Einstein Medium Sensitivity Survey sample (Gioia Luppino 1994) and of the CNOC survey (Carlberg et 11996).

$-$ 1224 is a rich galaxy cluster at redshift 0.302 that has been part of the Einstein Medium Sensitivity Survey sample (Gioia Luppino 1994) and of the CNOC survey (Carlberg et 1996).

Lombardi et ((2000) presented a detailed weak lensing analysis of the FORSI-VLT data.

Lombardi et (2000) presented a detailed weak lensing analysis of the FORS1-VLT data.

Figure | shows the X-ray Isophotes overplotted to the optical V-band image.

Figure \ref{opt_xray} shows the X-ray isophotes overplotted to the optical V-band image.

In the following we adopt the conversion 1aremin=376kpe (:= 0.302. If,=οτμkms.|!Μρο 1O,-21Oy-- 0.3) απά quote all the errors at Lo (68.3% confidence level).

In the following we adopt the conversion $1 \mbox{ arcmin} = 376 \mbox{ kpc}$ $z=0.302$ , $H_0 = 50 \, h_{50} \mbox{ km s}^{-1} \mbox{ Mpc}^{-1}$, $\Omega_{\rm m} = 1 - \Omega_{\Lambda} = 0.3$ ) and quote all the errors at $1 \sigma$ $68.3\%$ confidence level).

We retrieved the primary and secondary data products from the archive.

The exposure of 1224 was done on June 11. 2000 using the ACIS-I configuration.

The exposure of $-$ 1224 was done on June 11, 2000 using the ACIS-I configuration.

We reprocessed the levelz1 events file in the Very Faint Mode and. then. with the software 11.38: Townsley et 22000).

We reprocessed the level=1 events file in the Very Faint Mode and, then, with the software 1.38; Townsley et 2000).

The light curve was checked for high background flares that were not detected.

About [1.0ksec (out of [1.2 ksec. the nominal exposure time) were used and a total number of counts of about 20000 were collected from the region of interest in the 0.5-7 keV band.

About $44.0 \mbox{ ksec}$ (out of $44.2 \mbox{ ksec}$ , the nominal exposure time) were used and a total number of counts of about $20 \, 000$ were collected from the region of interest in the 0.5–7 keV band.

We used (v. 2.2: Elvis et 22002. in prep.)

We used (v. 2.2; Elvis et 2002, in prep.)

and our own routines to prepare the data to the imaging and spectral studies.

The X-ray center was fixed to the peak of the projected mass from weak lensing analysis (Lombardi. et 22000) at (RA. Dec: =(LOHLOM@32°68,12?39/58.87 ).

The X-ray center was fixed to the peak of the projected mass from weak lensing analysis (Lombardi et 2000) at (RA, Dec; ${} = (10^\mathrm{h} 10^\mathrm{m} 32\fs68, -12^{\circ} 39' 58.8")$ .

Note that the maximum value in à 5"-smoothed image of the cluster X-ray emission is at (RA. =(105109327LL.12739/55.6"). Le. less than 5 aresec apart from the adopted center.

Note that the maximum value in a $5\arcsec$ -smoothed image of the cluster X-ray emission is at (RA, ${} = (10^\mathrm{h} 10^\mathrm{m} 32\fs44, -12^{\circ} 39' 55.6")$, i.e. less than 5 arcsec apart from the adopted center.

With respect to the adopted center. a clear asymmetry in the surface brightness distribution is however detected. suggesting an excess in emission in the northern region (see Fig. 2)).

With respect to the adopted center, a clear asymmetry in the surface brightness distribution is however detected, suggesting an excess in emission in the northern region (see Fig. \ref{xray_asi}) ).

We detected extended emission at 20 confidence level up to 4.1 aremm(1.55 Mpe)and we were able to extract a total of four

We detected extended emission at $2 \sigma$ confidence level up to 4.1 arcmin$1.55 \mbox{ Mpc}$ )and we were able to extract a total of four

lines. as can be seen from Fig.

lines, as can be seen from Fig.

5 in MWT99..

5 in \cite{martini}.

The results obtained for this date are particularly uncertain. and. should be regarded with caution.

The results obtained for this date are particularly uncertain and should be regarded with caution.

They are based on rough estimates of the VR/ magnitudes made from the spectral observations.

They are based on rough estimates of the $VRI$ magnitudes made from the spectral observations.

Besides. judging from the estimated effective temperature the observations covered only the shortwavelength Wien's part of the spectrum.

Besides, judging from the estimated effective temperature the observations covered only the shortwavelength Wien's part of the spectrum.

The bulk of the energy of the object was presumably emitted in the infrared where no measurements were made.

Finally. our fits for this date. result from extrapolation beyond the range of the standard spectra (the latest types for which intrinsic colours are available are: Μό--7 for giants and M5-6 for supergiants).

Finally, our fits for this date result from extrapolation beyond the range of the standard spectra (the latest types for which intrinsic colours are available are: M6–7 for giants and M5–6 for supergiants).

Figure 3. shows the results of observations in. 1998. 1999 and 2003.

Figure \ref{sp03} shows the results of observations in 1998, 1999 and 2003.

Asterisks indicate the 2MASS measurements obtained on 18 May 1998.

Triangles show the DENIS results derived on 11 September 1999.

Circles represent the spectrum observed in May-September 2003 (see above for the sources fo the data).

First we discuss the observations obtained in 2003 as they cover the largest spectral range.

The whole spectrum. 1.8. all the circles in Fig. 3..

The whole spectrum, i.e. all the circles in Fig. \ref{sp03},

cannot be fitted with a single standard spectrum.

This can only be done for shorter wavelengths.

In Fig.

5 we show the best fits of the supergiant (full curve) and giant (dotted curve) spectra for the VR./..7 measurements.

\ref{sp03} we show the best fits of the supergiant (full curve) and giant (dotted curve) spectra for the $VR_cI_cJ$ measurements.

The parameters of the fits are given in Table 3..

The parameters of the fits are given in Table \ref{evol_t}.

The B magnitude has not been taken into account in the fitting procedure because of its significant uncertainty.

The $B$ magnitude has not been taken into account in the fitting procedure because of its significant uncertainty.

However. as can be seen from Fig. 3..

However, as can be seen from Fig. \ref{sp03},

it fits well the obtained spectra.

In the long wavlength range the H and. particularly. K magnitudes show a clear excess compared to the spectra fitted in the shorter wavelengths.

In the long wavlength range the $H$ and, particularly, $K$ magnitudes show a clear excess compared to the spectra fitted in the shorter wavelengths.

With the L and M magnitudes measured by BVAOA (not shown in Fig. 3))

With the $L$ and $M$ magnitudes measured by \cite{bva} (not shown in Fig. \ref{sp03}) )

one can easily conclude that the source of this excess dominates the brightness of the object in the infrared.

This infrared excess will be discussed in Sect. 6..

This infrared excess will be discussed in Sect. \ref{ire}.

The infrared observations displayed in Fig.

3. show that V4332 Ser evolved systematically between 1998 and 2003.

\ref{sp03} show that V4332 Sgr evolved systematically between 1998 and 2003.