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The motive for deriving upper limits is to determine whether or uot these stars ασ still be Al rich or whether they actually are Al normal ai the Al lines are undetectable because of | The motive for deriving upper limits is to determine whether or not these stars might still be Al rich or whether they actually are Al normal and the Al lines are undetectable because of |
power. | power. |
They one-bit sampled the data typically at intervals of 600 yes For this pulsar. | They one-bit sampled the data typically at intervals of 600 $\mu$ s for this pulsar. |
Phe data stream was written to tape for subsequent. oll-line analvsis. | The data stream was written to tape for subsequent off-line analysis. |
This analvsis involved. de-dispersing ancl folding the data at the topocentrie period. | This analysis involved de-dispersing and folding the data at the topocentric period. |
A digital correlator. the Caltech Fast Pulsar Timing Machine (EIDEM: Navarro 1994)). was in use between 1994 and 2001. | A digital correlator, the Caltech Fast Pulsar Timing Machine (FPTM; Navarro \nocite{nav94}) ), was in use between 1994 and 2001. |
lt had 128 Mllz of bandwidth with 128 frequency channels. | It had 128 MHz of bandwidth with 128 frequency channels. |
When operating in total power mode. two independent 128 MlIz bancs were available. | When operating in total power mode, two independent 128 MHz bands were available. |
When full Stokes parameters were recorded. however. onlv one band could be used. | When full Stokes parameters were recorded, however, only one band could be used. |
The correlator performed on-line pulse-folding and. cedispersion to produce a pulse profile with up to 1024 time bins per period. | The correlator performed on-line pulse-folding and dedispersion to produce a pulse profile with up to 1024 time bins per period. |
Further information for earlier observations can also be found in Wex et al. ( | Further information for earlier observations can also be found in Wex et al. ( |
1998) and Johnston et al. ( | 1998) and Johnston et al. ( |
2001). | 2001). |
The pulse profile of PSR 63 consists of two. almost equal-strength components. | The pulse profile of PSR $-$ 63 consists of two, almost equal-strength components. |
Each component has a steep edge anc a more slowly falling edge. | Each component has a steep edge and a more slowly falling edge. |
Manchester Johnston (1995) sugeestecd that the steep edges were the outside of a cone with large opening angle. | Manchester Johnston (1995) \nocite{mj95}
suggested that the steep edges were the outside of a cone with large opening angle. |
In order to obtain a good value for the dispersion measure. it is important that the profile be properly aligned over the entire. [frequency range between 0.66 and 13.6 Cllz. | In order to obtain a good value for the dispersion measure, it is important that the profile be properly aligned over the entire frequency range between 0.66 and 13.6 GHz. |
We chose the point michway between the mid-points of the steep outer edges as the fiducial point. | We chose the point midway between the mid-points of the steep outer edges as the fiducial point. |
At cach [requeney. a large number of profiles were summed. together to form a high. signal-to-noise template. | At each frequency, a large number of profiles were summed together to form a high signal-to-noise template. |
These templates are shown in Fig.1.. | These templates are shown in \ref{fg:std}. |
To obtain an accurate TOA we then eross-correlated individual observations with the relevant. template. | To obtain an accurate TOA we then cross-correlated individual observations with the relevant template. |
‘Table 2. lists the epoch of periastron for cach of the four orbits so far observed. | Table \ref{tb:gap} lists the epoch of periastron for each of the four orbits so far observed. |
Lt lists the total number of ΤΟΛΣ obtained during the orbit. and indicates the first detection of the pulsar after periastron and the final detection of the pulsar before it enters the eclipse. | It lists the total number of TOAs obtained during the orbit, and indicates the first detection of the pulsar after periastron and the final detection of the pulsar before it enters the eclipse. |
The eclipses of the pulsar. which last. for ~40 days around periastron make the timing difficult. | The eclipses of the pulsar, which last for $\sim$ 40 days around periastron make the timing difficult. |
Phe problem is exacerbated by the fact that DM changes are observed over a lew tens of days leading up to and immediately following the eclipse clue to the changing line of sight intersecting the 3e star wind. | The problem is exacerbated by the fact that DM changes are observed over a few tens of days leading up to and immediately following the eclipse due to the changing line of sight intersecting the Be star wind. |
Fhese DAL variations need to be removed to obtain a good timing solution. and this involves making observations at several dillerent frequencies as near to simultaneously as possible. | These DM variations need to be removed to obtain a good timing solution, and this involves making observations at several different frequencies as near to simultaneously as possible. |
Multi-[requeney observations were therefore mace before and after the 1994. 1997. and | Multi-frequency observations were therefore made before and after the 1994, 1997 and |
Ale. Na. ancl Al weren't though to be processed around the H shell. aud any variations iu them were taken as evideuce that some kind of primordial polluion allectecl the surface abuudaices Costa1981 .. | Mg, Na, and Al weren't thought to be processed around the H shell, and any variations in them were taken as evidence that some kind of primordial pollution affected the surface abundances \citep[see, e.g.,][]{CD81}. |
Continued work on keγια uclear reaction rates (CharipagneetHiacisetal.1996). . however. suggestMODa hat these elements could be yrocessecl around the H shell uuder the saue conditious that the C 1id ON nuclear cycles operaed. | Continued work on key nuclear reaction rates \citep{Champagne98,DD90,Iliadis90,
CBS93,Blackmon95,Iliadis96}, however, suggested that these elements could be processed around the H shell under the same conditions that the CN and ON nuclear cycles operated. |
Usine these results. as wel as the wicely accepted rates of Catelin&Fowler(1985).. separae groups showed that it is [xsible ο account qualitatively for the observed variations that slowed Na. Al. and N anticoeated with C. O. and. in some cases. A[n]0 (Laugeretal.1993:CavalloDeuisseukov&Weiss1996:Cavalloetal.1998:Denissenkov 1998). | Using these results, as well as the widely accepted rates of \citet{CF88}, separate groups showed that it is possible to account qualitatively for the observed variations that showed Na, Al, and N anticorrelated with C, O, and, in some cases, Mg \citep{LHS93, CSB96, DW96, CSB98, DDNW98}. |
. The challeipe has always been descjbiug the resUtsquantitatively: in particular. produciug [AI/Fe] as higl as 1EE dex without over»oduciig [Na/Fe]. and depleting ?!Mg to the observed levels in M13 1996b).. all while rellaining witun the acceptable proton-capture rates (Langeretal.1997:;igulo1999:Poweletal.Iiadis 2001). | The challenge has always been describing the results; in particular, producing [Al/Fe] as high as 1.5 dex without overproducing [Na/Fe], and depleting $^{24}$ Mg to the observed levels in M13 \citep{S96b}, all while remaining within the acceptable proton-capture rates \citep{LHZ97,NACRE,Powell99,UNC}. |
. Despite auy latiude allorded by the react rate uucertaiuties (see.e.g..Cavalloetal.1995).. the mixing theory 5ill relies on nou-solar abialice ratios in the star prior to mixitο (Deuissenkovetal.1998:Cavalo&Nagar2000).. thus. a least partly relying oi primordial influeuces. | Despite any latitude afforded by the reaction rate uncertainties \citep[see, e.g.,][]{CSB98}, the mixing theory still relies on non-solar abundance ratios in the star prior to mixing \citep{DDNW98,CN2000}, thus, at least partly relying on primordial influences. |
Theories othe “ilau mericlloual circulation have beer put forth (Langeretal.1997:Fuji1roto1999:Aikaw1l.FujimoWeiss 2001).. bu a cetailed cliscussion of each is bevo( he intent oL this paper. | Theories other than meridional circulation have been put forth \citep{LHZ97,FAK99,
AFK2001,DW2001}, but a detailed discussion of each is beyond the intent of this paper. |
Regardless of the plNsles elünd any mixing mec!1sin. the αιestion still remains: are he Al id Na. Mg) varlatious cause| by mixing. primordial soces. OF acombination of both? | Regardless of the physics behind any mixing mechanism, the question still remains: are the Al (and Na, Mg) variations caused by mixing, primordial sources, or a combination of both? |
We mielit abe (lO aliswel this question by looking at another ¢[n]0 outstauclue problem in globular cluster ronony. namely. the seconcd-parameter elect. | We might be able to answer this question by looking at another long outstanding problem in globular cluster astronomy, namely, the second-parameter effect. |
First poi1ed out by Saudage&Wileev(1967) aud 1denBerel 1967)..11e secoli-parameer elect refer:« o the phe101uenon where 1ie (HB of two clusters witl1 slinilar metallicity (te first parapeter) have ma‘keclly differeut COor distribu10s. | First pointed out by \citet{SW67} and \citet{vdB67}, the second-parameter effect refers to the phenomenon where the horizontal-branches (HB) of two clusters with similar metallicity (the first parameter) have markedly different color distributions. |
Possible secoxl paratjeters. that have beeu investigated incldle age. initial relitun abuud:uice. (ΝΟ abuudaue. ancl iiass loss (see.e.g..Faulkueetal. 1998).. aLOig others. but uoje Is appicable to all clusters. | Possible second parameters that have been investigated include age, initial helium abundance, CNO abundance, and mass loss \citep[see, e.g.,][]{Faulkner66,Renzini77,Chaboyer98}, among others, but none is applicable to all clusters. |
One recent suggesMODion Lypothesizes hat i ‘cleep mixii& (1e.. inixine 11at penetrates the H shell) occurs. then helium wil be brought to he surface allecting the HB morphology by making mixed stars both bluer aud b‘ighter (Sweigart 1997a.b). | One recent suggestion hypothesizes that if deep mixing (i.e., mixing that penetrates the H shell) occurs, then helium will be brought to the surface affecting the HB morphology by making mixed stars both bluer and brighter (Sweigart 1997a,b). |
Uufortunatev. helium cannot be measured in RGB stars because of their low si‘face temperaturen. aud helium. settliug ou the HB precludes au accurate measurement in the hotter stars. | Unfortunately, helium cannot be measured in RGB stars because of their low surface temperatures, and helium settling on the HB precludes an accurate measurement in the hotter stars. |
However. uodels by Cavaloοἱal.(1998).. which use standard (albeit. uncertain) reaction ‘ates. show that aluimninu can be produced ouly iu the H shell of giants within the last inagnittcle of the RGB. inplyiug that ai iucrease in helium in the envelope must also be accompanied bv an increase ln aluimninn. | However, models by \citet{CSB98}, which use standard (albeit, uncertain) reaction rates, show that aluminum can be produced only in the H shell of giants within the last magnitude of the RGB, implying that an increase in helium in the envelope must also be accompanied by an increase in aluminum. |
From this we can postulate that. if [AI/Fe] variations are produced inernally aud uot orimorcially. Al could be a good surrogate to measure He mixing on the bright ROB. aud if He ulxiug is indeed the secoucl parameter. a relationship should exist between the ratio of Al-strone | From this we can postulate that, if [Al/Fe] variations are produced internally and not primordially, Al could be a good surrogate to measure He mixing on the bright RGB, and if He mixing is indeed the second parameter, a relationship should exist between the ratio of Al-strong |
We now attempt to crudely estimate the 350yr source counts at our typical observed Hux density. even though the SUARC-LE data are not blank-field observations. | We now attempt to crudely estimate the $350\,\mathrm{\mu m}$ source counts at our typical observed flux density, even though the SHARC-II data are not blank-field observations. |
We place an upper limit on the source counts using the number of detections acquired in the observed area: one would expect to do than this in a blank-felel survey. since. here known SAIGs were observed. | We place an upper limit on the source counts using the number of detections acquired in the observed area; one would expect to do than this in a blank-field survey, since here known SMGs were observed. |
Given a total observed. area of 48.3aremin? and seven detectionsabove a 350jin. [ux density of 225 muda. we estimate Ας8)500deg | Given a total observed area of $48.3\,\mathrm{arcmin}^{2}$ and seven detectionsabove a $350\,\mathrm{\mu m}$ flux density of $\simeq25$ mJy, we estimate $N(>\!S)\lesssim500\,\mathrm{deg}^{-2}$. |
We estimate a lower limit on the source counts hy applying the SILABC-HE detection rate of SbO/m. sources to. the whole SHADES area: one would. expect to do at least as well in a blank-lielel search. | We estimate a lower limit on the source counts by applying the SHARC-II detection rate of $850\,\mathrm{\mu m}$ sources to the whole SHADES area; one would expect to do at least as well in a blank-field search. |
We estimate a lower limit of AN(S)200ceg eiven à SILABC-LLE detection success rate of 7/24 and a total of 120 SLLADIES sources found in ~T20aremin. | We estimate a lower limit of $N(>\!S)\gtrsim200\,\mathrm{deg}^{-2}$, given a SHARC-II detection success rate of 7/24 and a total of 120 SHADES sources found in $\simeq720\,\mathrm{arcmin}^{2}$. |
Note that we have neglected the possibility of enhanced density from clustering. | Note that we have neglected the possibility of enhanced density from clustering. |
“Phe limits derived here are consistent with the predictions from Lagacheetal.(2004) and scenario E from the semi-analytie models of Ciuiderdonictal.(1998). (see Fig. 3)). | The limits derived here are consistent with the predictions from \citet{Lagache2004} and scenario E from the semi-analytic models of \citet{Guiderdoni} (see Fig. \ref{fig:350bf}) ). |
Although crude. this is the best available estimate of the 350yma source counts at these Dux densities. | Although crude, this is the best available estimate of the $350\,\mathrm{\mu m}$ source counts at these flux densities. |
Khanctal.(2007). also report the 350p/m source counts above 13muimiJv. from a deep survey with SILABC-HI. | \citet{Khan} also report the $350\,\mathrm{\mu m}$ source counts above mJy from a deep survey with SHARC-II. |
Large surveys planned. with the Balloon-borne Large Aperture Submm Telescope (BLAST: etal. 2004). (Pilbratt2003).. SCUBA-2 (Lollandetal. 2006)... anc (Lauber2004) will be able to provide further constraints on the source counts at shorter submim wavelengths and over a wider dvnamic range of [ux densities. | Large surveys planned with the Balloon-borne Large Aperture Submm Telescope (BLAST; \citealt{Devlin}) ), \citep{Pilbratt}, SCUBA-2 \citep{Holland2006}, and \citep{Planck} will be able to provide further constraints on the source counts at shorter submm wavelengths and over a wider dynamic range of flux densities. |
The SEDs of SMCGs is dominated by thermal emission from cold. dust. | The SEDs of SMGs is dominated by thermal emission from cold dust. |
SILARC-IHE photometry of the SLADE sources can determine the apparent temperature of the dust. | SHARC-II photometry of the SHADES sources can determine the apparent temperature of the dust. |
In. conjunction with knowledge of the redshift. this allows inference of dust masses. FUR luminosities. and SERs. allowing one to place these objects in context with other populations of high-redshift star-forming galaxies and CN. | In conjunction with knowledge of the redshift, this allows inference of dust masses, FIR luminosities, and SFRs, allowing one to place these objects in context with other populations of high-redshift star-forming galaxies and AGN. |
The shape of a luminous clusty galaxy SED is well approximated by a mocified blackbody spectrum described bv the dust. temperature. Z4. and dust. emissivity £O. | The shape of a luminous dusty galaxy SED is well approximated by a modified blackbody spectrum described by the dust temperature, $T_\mathrm{d}$, and dust emissivity $\epsilon \propto \nu^{\beta}$ . |
where S lies in a physically plausible range of 12 (Llildebrand 1983).. | where $\beta$ lies in a physically plausible range of 1–2 \citep{Hildebrand1983}. . |
Phere is a degencracy between Zi and ? which cannot be disentangled by our data | There is a degeneracy between $T_\mathrm{d}$ and $\beta$ which cannot be disentangled by our data |
We again measure distances in units of GM/c?, with ἃ:=a/(Gm/c?) and d:-d/(Gm/c?).Typical interesting values are ázzafew and d~fewtens. | We again measure distances in units of $GM/c^2$, with $\hat{a} := a/(G m/c^2)$ and $\peri := d/(G m/c^2)$.Typical interesting values are $\hat{a}\approx{\rm a~few}$ and $\peri\approx{\rm few~tens}$. |
Therefore, and We then obtain the ratio of the two timescales, For a self-gravitating cluster, we can rewrite this in terms of N, and R, using Viazc, This quantity can be interpreted as the probability that a relativistic binary has a close encounter with a single object before it merges. | Therefore, and We then obtain the ratio of the two timescales, For a self-gravitating cluster, we can rewrite this in terms of $N$, and $R$, using $V_{\rm rel}\approx \sigma$, This quantity can be interpreted as the probability that a relativistic binary has a close encounter with a single object before it merges. |
The total number of mergers that can occur in the evolution of a cluster of N objects is Nmerg<N, with Nmerg=N only possible if all objects merge togethera | The total number of mergers that can occur in the evolution of a cluster of $N$ objects is $N_{\rm merg}\le N$, with $N_{\rm merg}= N$ only possible if all objects merge together. |
Hence, the total number of [Lee]relativistic[1993; single-binaryetal] [Kupi2006)..interactions over the lifetime of a cluster (evolving through a succession of binary mergers) is In this work we have addressed the formation of systems of three BHs in the strong gravity regime. | Hence, the total number of relativistic single-binary interactions over the lifetime of a cluster (evolving through a succession of binary mergers) is In this work we have addressed the formation of systems of three BHs in the strong gravity regime. |
For that we have first studied the probability that three BHs interact in a dense stellar cluster and we conclude that it is totally negligible. | For that we have first studied the probability that three BHs interact in a dense stellar cluster and we conclude that it is totally negligible. |
We have then addressed the possibility that a binary of BHs which has previously formed in the cluster interacts relativistically with a third BH. | We have then addressed the possibility that a binary of BHs which has previously formed in the cluster interacts relativistically with a third BH. |
We that the stellar system harbouring the BHs needs to have judgeunachievable densities. | We judge that the stellar system harbouring the BHs needs to have unachievable densities. |
Based on simple physical arguments, we have established that the time scales for a triple relativistic encounter to occur in a cluster of stellar-mass compact objects is extremely long. | Based on simple physical arguments, we have established that the time scales for a triple relativistic encounter to occur in a cluster of stellar-mass compact objects is extremely long. |
We recall that we consider two extreme cases. | We recall that we consider two extreme cases. |
In the first situation, we neglect the existence (and formation) of binaries. | In the first situation, we neglect the existence (and formation) of binaries. |
Hence, we consider that three single objects have to find themselves, by chance, within a few (tens of) Schwarzschild radii of each other. | Hence, we consider that three single objects have to find themselves, by chance, within a few (tens of) Schwarzschild radii of each other. |
In this case, we have admitted that the cluster cannot survive (with a high stellar density) for more than about 100 relaxation time. | In this case, we have admitted that the cluster cannot survive (with a high stellar density) for more than about 100 relaxation time. |
Indeed, in such a long time scale, most of the cluster would expand to lower and lower densities and a very significant fraction of the object would escape, with only a very small number of objects getting closer and closer to provide energy for this evolutionHut003). | Indeed, in such a long time scale, most of the cluster would expand to lower and lower densities and a very significant fraction of the object would escape, with only a very small number of objects getting closer and closer to provide energy for this evolution. |
. The second (much idealized) case is that of a [&cluster made mostly of binaries. | The second (much idealized) case is that of a cluster made mostly of binaries. |
In that case, one can hope that it would suffice for an object to interact closely with a binary but in order for the interaction to be relativistic for the three objects, the binary must be so tight that its lifetime is limited by emission of gravitational waves. | In that case, one can hope that it would suffice for an object to interact closely with a binary but in order for the interaction to be relativistic for the three objects, the binary must be so tight that its lifetime is limited by emission of gravitational waves. |
Accordingly, we consider that the lifetime of the whole cluster is limited by the successive merger of binaries. | Accordingly, we consider that the lifetime of the whole cluster is limited by the successive merger of binaries. |
Any real cluster would present a situation which is somewhat in between these two extremes. | Any real cluster would present a situation which is somewhat in between these two extremes. |
In particular, the evolution of a cluster made of single objects would naturally lead to the formation of binaries during core collapseHut|2003). | In particular, the evolution of a cluster made of single objects would naturally lead to the formation of binaries during core collapse. |
. We stress that we have made a large [Heggienumber of& simplifications in our estimates but always in such a way as to overestimate the rate of triple relativistic events. | We stress that we have made a large number of simplifications in our estimates but always in such a way as to overestimate the rate of triple relativistic events. |
For instance, we have assumed that all the binaries in a cluster are relativistic. | For instance, we have assumed that all the binaries in a cluster are relativistic. |
This limits their lifetime but non-relativistic binaries are useless for our purpose. | This limits their lifetime but non-relativistic binaries are useless for our purpose. |
With figure[I], we can estimate what conditions are required for at least one such encounter to take place during the lifetime of the cluster. | With figure \ref{fig.NR}, we can estimate what conditions are required for at least one such encounter to take place during the lifetime of the cluster. |
For this figure, we have assumed m=10M and d=á104. | For this figure, we have assumed $m=10\,\Msun$ and $\peri=\hat{a}=10^4$. |
The latter values correspond to encounters that are only weakly relativistic. | The latter values correspond to encounters that are only weakly relativistic. |
Even with such values, the figure shows that most of the parameter space for ΛΑsingle=1 Or N3pin21 is excluded, either because the cluster, as a whole, would be a massive black hole (for large N and small R) or because the cluster would have such a small 2-body relaxation time that it wouldn't have time to form (for smaller N and small R). | Even with such values, the figure shows that most of the parameter space for $N_{3,\,\rm
single}\gtrsim 1$ or $N_{3,\,\rm bin}\gtrsim 1$ is excluded, either because the cluster, as a whole, would be a massive black hole (for large $N$ and small $R$ ) or because the cluster would have such a small 2-body relaxation time that it wouldn't have time to form (for smaller $N$ and small $R$ ). |
Indeed, the evolution of massive stars into compact objects (neutron stars or black holes) requires at least 3 million years. | Indeed, the evolution of massive stars into compact objects (neutron stars or black holes) requires at least 3 million years. |
Because of these constraints, it appears that clusters hosting triple relativistic encounters have to be made of at least 10? compact objects concentrated within a region smaller than 10?pc. | Because of these constraints, it appears that clusters hosting triple relativistic encounters have to be made of at least $10^8$ compact objects concentrated within a region smaller than $10^{-3}\,{\rm pc}$. |
In fact, for N~105, the size has to be of order 107pc. | In fact, for $N\approx10^8$, the size has to be of order $10^{-4}\,{\rm pc}$. |
The corresponding number density is comprised between 10!7 and 10?pc. | The corresponding number density is comprised between $10^{17}$ and $10^{19}\,{\rm pc}^{-3}$. |
Such values are beyond observed ones by many orders of magnitude. | Such values are beyond observed ones by many orders of magnitude. |
For instance, the stellar density in Galactic globular clusters is, at most, of the order of 105pc? | For instance, the stellar density in Galactic globular clusters is, at most, of the order of $10^{5}\,{\rm pc}^{-3}$. |
Already the necessary number mwgc.dat)mainBodyCitationEnd1958]Harris96.of compact objects is much| larger than what one can expect in the kind of clusters that exist. | Already the necessary number of compact objects is much larger than what one can expect in the kind of clusters that exist. |
A globular cluster might contain up to 107 stars but only a very small fraction of them would become BHs. | A globular cluster might contain up to $10^7$ stars but only a very small fraction of them would become BHs. |
This number fraction f depends on the initial mass function (IMF) of high mass stars. | This number fraction $f$ depends on the initial mass function (IMF) of high mass stars. |
Some galactic nuclei seem to be top-heavy aT]D007),, so that in principle f ranges between 107? (Manessand et107, yielding, at most, N=10? BHs in very large cluster. | Some galactic nuclei seem to be top-heavy , so that in principle $f$ ranges between $10^{-3}$ and $10^{-2}$ , yielding, at most, $N=10^5$ BHs in very large globular cluster. |
A globulargalaxy contains a much larger number of compact objects | A galaxy contains a much larger number of compact objects |
galaxies. | galaxies. |
Using spatially resolved data for the LMC. I suggest that dust geometry and properties. coupled with a small contribution from older stellar populations. contribute to deviations from the starburst galaxy J-Ayuy correlation. | Using spatially resolved data for the LMC, I suggest that dust geometry and properties, coupled with a small contribution from older stellar populations, contribute to deviations from the starburst galaxy $\beta$ correlation. |
Neither rest frame UV-optical colors nor significantly help in constraining the UV attenuation. | Neither rest frame UV-optical colors nor significantly help in constraining the UV attenuation. |
These results argue that the estimation of SF rates from rest-frame UV and optical data alone is subject to large (factors of at least a few) systematic uncertainties because of dust. whichcannot be reliably corrected for using only UV/optical diagnostics. | These results argue that the estimation of SF rates from rest-frame UV and optical data alone is subject to large (factors of at least a few) systematic uncertainties because of dust, which be reliably corrected for using only UV/optical diagnostics. |
I wish to thank Kurt Adelberger. Daniela Calzetti. Betsy Barton Gillespie. Karl Gordon. Rob Kennicutt. Mark Seibert. Richard Tuffs. and Dennis Zaritsky for useful discussions and suggestions. | I wish to thank Kurt Adelberger, Daniela Calzetti, Betsy Barton Gillespie, Karl Gordon, Rob Kennicutt, Mark Seibert, Richard Tuffs, and Dennis Zaritsky for useful discussions and suggestions. |
Special thanks go to the anonymous referee for their careful suggestions. | Special thanks go to the anonymous referee for their careful suggestions. |
This work was supported by NASA grant NAGS-8426 and NSF grant AST-9900789. | This work was supported by NASA grant NAG5-8426 and NSF grant AST-9900789. |
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