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Ou the other hand. our modeling ou the B/D of Sa spirals is a coustaut 0.5. which might © too simplified. | On the other hand, our modeling on the $B/D $ of Sa spirals is a constant 0.5, which might be too simplified. |
Iu the study of M6. all the S0/Sa/Sab ealaxies are erouped as Sa type. | In the study of M06, all the S0/Sa/Sab galaxies are grouped as Sa type. |
Among three sub-types. he earlier type galaxies. e.g. SO. having svstematicallv areer D/D. are also svetematically brighter. | Among three sub-types, the earlier type galaxies, e.g. S0, having systematically larger $B/D$, are also systematically brighter. |
Therefore. roni low Vias to high Vinax galaxies. there is actually a svsteimiatical change of B/D. which will also shallow the slope of TER. | Therefore, from low $\Vmax$ to high $\Vmax$ galaxies, there is actually a systematical change of $B/D$, which will also shallow the slope of TFR. |
By introducing a svstematical change of DD as function of Vyas. We can iu principle reproduce he slope of Sa spirals as observed. | By introducing a systematical change of $B/D$ as function of $\Vmax$, we can in principle reproduce the slope of Sa spirals as observed. |
However. we prefer rot to tune our model to reproduce this relation with a cost of introducing more unucertaimties. | However, we prefer not to tune our model to reproduce this relation with a cost of introducing more uncertainties. |
Comparing with the unucertaimties in the modeling of he TER slope. the zero-poiut is quite robust. | Comparing with the uncertainties in the modeling of the TFR slope, the zero-point is quite robust. |
Moreover. uanv studies of the morphological depeudeuce of the TFRs oulv report a global shift of the zero-point. e.g. Ciovanelhetal.(1997):Russell(2001.2008) (sce text section). | Moreover, many studies of the morphological dependence of the TFRs only report a global shift of the zero-point, e.g. \citet{Giovanelli97,Russell04,Russell08} (see next section). |
Therefore. in the following section. we xwanmeterize the morphological depeudeuce of the TFRs only with the shift ofthe zero-point AM. | Therefore, in the following section, we parameterize the morphological dependence of the TFRs only with the shift of the zero-point $\Delta M$. |
We choose the zero-point shift AAS of the TFRs at Vinx=200]anst. where the correspouding absolute magnitude is roughly the AL. of the Iuninositv functiou of spiral galaxies and where the number couuts of ealaxies iu a fiux-liuited sample normally peaks. | We choose the zero-point shift $\Delta M$ of the TFRs at $\Vmax =200\kms$, where the corresponding absolute magnitude is roughly the $M_*$ of the luminosity function of spiral galaxies and where the number counts of galaxies in a flux-limited sample normally peaks. |
Iu this case. AM=A of Equ. | In this case, $\Delta M=\Delta \beta$ of Equ. |
1. | 1. |
We show the ΔΑ between Sb aud Se spirals in the top panel of Fig. 3.. | We show the $\Delta M$ between Sb and Sc spirals in the top panel of Fig. \ref{ZP_TFR}, |
whereas the AAL between Sa aud Se spirals is shown iu the bottom panel. | whereas the $\Delta M$ between Sa and Sc spirals is shown in the bottom panel. |
The model predicted AA in different wavebiuds are connected as a function of their effective waveleugths with μπας, | The model predicted $\Delta M$ in different wavebands are connected as a function of their effective wavelengths with lines. |
The wavebauds iuclude C.B.V.RDAIT.NK. aud the wavelength ranges from 0.33 to 2.2 micron. | The wavebands include $U,B,V,R,I,J,H,K$ and the wavelength ranges from 0.33 to 2.2 micron. |
The observed difference of AA at των=200hans3 in differcut bauds found iu the literature are plotted against their effective wavelcneths. | The observed difference of $\Delta M$ at $\Vmax=200\kms$ in different bands found in the literature are plotted against their effective wavelengths. |
Results from different authors are labeled with different sviubol types. | Results from different authors are labeled with different symbol types. |
The references aud details of these morphology dependent TFRs are listed in Table 1. | The references and details of these morphology dependent TFRs are listed in Table 1. |
A few other studies in the literature are not quoted in Table 1 aud Fig. 3.. | A few other studies in the literature are not quoted in Table 1 and Fig. \ref{ZP_TFR}, |
meludiug Rubinetal. (1985).. Caovancliietal.(1997). aud the TER. of Sb spirals of Sandage(2000). | including \cite{Rubin85}, \cite{Giovanelli97} and the TFR of Sb spirals of \cite{Sandage00}. |
. Rubinetal.(1985) found the magnitude differences AAL between Sa aud Sc spirals are as high as 2 mag in 2 baud aud 1 mas in ZI baud. whose nunber of each type galaxies is liuüted(« 20) and without error estimation quoted for the parameters of TFRs. | \cite{Rubin85} found the magnitude differences $\Delta M$ between Sa and Sc spirals are as high as 2 mag in $B$ band and 1 mag in $H$ band, whose number of each type galaxies is $<20$ ) and without error estimation quoted for the parameters of TFRs. |
The 7 baud data of Caovanellietal.(1997) has been expauded and re-analyzed by ALOG auc their results are generally cousisteut. | The $I$ band data of \cite{Giovanelli97} has been expanded and re-analyzed by M06 and their results are generally consistent. |
The TFR of Sb spirals in Sandage(2000) is arbitrarily ucelected. where its zero-point is even lower than Sc spirals. ic. AA(Sb-Sc)« 0. contracictorv to most of the other studies. | The TFR of Sb spirals in \cite{Sandage00} is arbitrarily neglected, where its zero-point is even lower than Sc spirals, i.e. $\Delta M$ $<0$ , contradictory to most of the other studies. |
The solid Lunes iu Fig. | The solid lines in Fig. |
3. show predictious frou the K91 model. ie. the model with 7= 3.5.30€x for Sa.Sb.Se spirals respectively. | \ref{ZP_TFR} show predictions from the K94 model, i.e. the model with $\tau=3,5,30$ Gy for Sa,Sb,Sc spirals respectively. |
The shadowed reeious€ show the rauges of inodel predicted AAS when τ ovaries in its lo rauge. | The shadowed regions show the ranges of model predicted $\Delta M$ when $\tau$ varies in its $\sigma$ range. |
As we can sec. the R91 model over-precdicts the differences of the zero-points significantly for both Sb/Se and SafSe pairs. | As we can see, the K94 model over-predicts the differences of the zero-points significantly for both Sb/Sc and Sa/Sc pairs. |
The average observed zero-point differences in uear-infrared bands are AAL(Sb-Se)~0.15 mimag aud AAL(Sa- Sc)50.201umniag. whereas the model prediction is as high as AAL(Sb-Sce)~0. ΕΕ and AAL(Sa-Se}~0.60 manag. | The average observed zero-point differences in near-infrared bands are $\Delta
M$ $\sim$ mag and $\Delta M$ $\sim$ mag, whereas the model prediction is as high as $\Delta M$ $\sim$ mag and $\Delta
M$ $\sim$ mag. |
That means. if the differences of the stellar populations of the disks of differeut type spirals are as that suggested by K91. the slüft of the zero-point of the TFRs would be much larger than observed. | That means, if the differences of the stellar populations of the disks of different type spirals are as that suggested by K94, the shift of the zero-point of the TFRs would be much larger than observed. |
With the disk star formation time scale 7 approaching its upper rauge(the lower boundary of the shadowed reeion). the discrepancy between the model predicted AM aud the observations becomes sinaller. | With the disk star formation time scale $\tau$ approaching its upper range(the lower boundary of the shadowed region), the discrepancy between the model predicted $\Delta M$ and the observations becomes smaller. |
This result prompts us to consider an extreme case, 7=306v for both Sa aud Sb disks. | This result prompts us to consider an extreme case, $\tau=30$ Gy for both Sa and Sb disks. |
Iu this case. the stellar populatious of the disks of different type spirals are the same. while the differeut global colors of differcut tvpoe spirals oulv originate frou the bulge disk composition effect. | In this case, the stellar populations of the disks of different type spirals are the same, while the different global colors of different type spirals only originate from the bulge disk composition effect. |
This scenario is consistent with the results of Dewvereux&Young(1991). | This scenario is consistent with the results of \citet{Devereux91}. |
. To distinguish it from the NOL model. we refer to this scenario(7=30 Cx for all type disks) as the ‘composition model below. | To distinguish it from the K94 model, we refer to this $\tau=30$ Gy for all type disks) as the `composition' model below. |
For the "composition model. the model predicted AAL as function of the effective wavelength is shown as the dotted lines in Fig. 3.. | For the `composition' model, the model predicted $\Delta M$ as function of the effective wavelength is shown as the dotted lines in Fig. \ref{ZP_TFR}. |
Surprisingly. the predicted AALS from this model. especially in mear-iutrared bonds. is eenerallv cousistent with observations. either for Sb/Sc or Sa/Se pairs. | Surprisingly, the predicted $\Delta M$ from this model, especially in near-infrared bands, is generally consistent with observations, either for Sb/Sc or Sa/Sc pairs. |
The predicted AA/ in DB baud is sinaller than that observed. | The predicted $\Delta M$ in $B$ band is smaller than that observed. |
A possible| solution to this discrepancy is the dust extinction which has not becu aken iuto account iu our model. | A possible solution to this discrepancy is the dust extinction which has not been taken into account in our model. |
If the face-on dust extinction of earlier type spirals is more significant. he ΔΑ in blue baud will be larecr than now we πα detailed discussions iu Section ??)). | If the face-on dust extinction of earlier type spirals is more significant, the $\Delta M$ in blue band will be larger than now we predicted(see detailed discussions in Section \ref{dust}) ). |
Finally. it is worth meutioning that the AA between different spiral types is nof contributed by the stellar »pulatiou alone but composed by both the dyvuanuics and stellar population. | Finally, it is worth mentioning that the $\Delta M$ between different spiral types is not contributed by the stellar population alone but composed by both the dynamics and stellar population. |
As we have shown iu section ??.. or the galaxies with the same stellar mass 3«101"AZ... he Vas of a Sa(Sb) spiral is about 1.5(1.0) percent üeher than Se spiral. which corresponds to the AAS ~(1.010003) minae. independent of the wavebauds. | As we have shown in section \ref{sec_RC}, for the galaxies with the same stellar mass $3\times10^{10}M_\odot$, the $\Vmax$ of a Sa(Sb) spiral is about 1.5(1.0) percent higher than Sc spiral, which corresponds to the $\Delta M$ $\sim0.04(0.03)$ mag, independent of the wavebands. |
This contribution is shown as two dashed horizoutal lines in the top aud bottom panels of Fig. 3.. | This contribution is shown as two dashed horizontal lines in the top and bottom panels of Fig. \ref{ZP_TFR}. |
However. as we can see. the stellar population is still the domiuaut contributor to the morphological depeudence of the TER. | However, as we can see, the stellar population is still the dominant contributor to the morphological dependence of the TFR. |
There are some uncertainties in our modeling of both dynamics and stellar population of the spiral galaxies. e.g. the scatters of iiodel paraiecter. the diverse bulge properties and the internal dust extinction ote. | There are some uncertainties in our modeling of both dynamics and stellar population of the spiral galaxies, e.g. the scatters of model parameter, the diverse bulge properties and the internal dust extinction etc. |
We discuss these issues below. | We discuss these issues below. |
Tn our modeling. we oulv takethe typical values for each model parameter aud do not consider their scatters except the kev parameter 7. However. all these model parameters show scatters as sugeested by either nunierie sauulations or observations. e.g. Mo&Mao (2002).. | In our modeling, we only takethe typical values for each model parameter and do not consider their scatters except the key parameter $\tau$ However, all these model parameters show scatters as suggested by either numeric simulations or observations, e.g. \citet{Mo00,Jing00,Shen02}. . |
Tf the scatters of model parameters are independent variables aud do not | If the scatters of model parameters are independent variables and do not |
Deupree1998 Arnett(1994) Bazan&Arnett(1994).nett(1998) Arnett(1994). (10° 10°s. Arnett(1996))). Bazàn&ArnettArnett(1998) (Livne1993)). Glasner Tuchman(1997) Asida(2000). (2000) Smagorinsky(1963) | \cite{dpr98} \cite{arn94} \cite{ba94,ba98}
\cite{arn94} $10^3$ $10^5\rm\ s$ \cite{arn96}) \cite{ba94,ba98} \cite{lvn93}) \cite{gl95} \cite{at97} \cite{asd00} \cite{asd00} \cite{smg63} |
The slopes predicted by our caleulations [or different values of the shock velocity are shown in Table 1 [or &=0.01 and agree well with those of Nirk et al. ( | The slopes predicted by our calculations for different values of the shock velocity are shown in Table 1 for $\sigma=0.01$ and agree well with those of Kirk et al. ( |
2000). | 2000). |
In Fig. | In Fig. |
5. we also plot the distribution functions obtained for all (he cases reported in Table 1 (the upper panel refers to the first [our lines in Table 1. while the lower panel refers to the relativistic regime. namelv the last four lines in Table 1). | \ref{fig:anis} we also plot the distribution functions obtained for all the cases reported in Table 1 (the upper panel refers to the first four lines in Table 1, while the lower panel refers to the relativistic regime, namely the last four lines in Table 1). |
This figure shows the expected phenomenon of increasing anisotropy in the distribution funtion when (he shock speed increases: for non-relativistic speeds the distribution hunction is almost perfectly independent of the pitch angle ji but it becomes more and more anisotropic in the trans-relativistic regime and in the fully relativistic regime. | This figure shows the expected phenomenon of increasing anisotropy in the distribution funtion when the shock speed increases: for non-relativistic speeds the distribution function is almost perfectly independent of the pitch angle $\mu$, but it becomes more and more anisotropic in the trans-relativistic regime and in the fully relativistic regime. |
A necessary condition for the SPAS regime to be atwork is that σ Ηστ. | A necessary condition for the SPAS regime to be atwork is that $\sigma \ll 1/4\gamma_{sh}^2$ . |
This | This |
We previously reported in Letaweetal.(2009) the possible detection of a second active nucleus in the companion galaxy. hidden by large dust clouds. | We previously reported in \cite{letg09} the possible detection of a second active nucleus in the companion galaxy, hidden by large dust clouds. |
This tentative detection was based on HST/NICMOS H-band and VLT/ISAAC K-band observations. | This tentative detection was based on HST/NICMOS H-band and VLT/ISAAC K-band observations. |
We looked for a point source in the J-band image of the companion galaxy and could not detect any. | We looked for a point source in the J-band image of the companion galaxy and could not detect any. |
This is however compatible with an AGN hidden behind a dust cloud. the extinction in the J-band being sufficient to make this point source disappear almost completely ( the estimated extinction Ay=Ι5 converts to A;=7.2. as the observed J-band corresponds roughly to restframe If confirmed. the presence of a second AGN in the companion galaxy would be difficult to explain if the latter was built up only by star formation induced by a jet originating from the main QSO. as suggested in Elbazetal.(2009). | This is however compatible with an AGN hidden behind a dust cloud, the extinction in the J-band being sufficient to make this point source disappear almost completely ( the estimated extinction $A_V \simeq 15$ converts to $A_I \simeq 7.2$, as the observed J-band corresponds roughly to restframe If confirmed, the presence of a second AGN in the companion galaxy would be difficult to explain if the latter was built up only by star formation induced by a jet originating from the main QSO, as suggested in \cite{elbaz}. |
. The detection of a plausible host rules out the scenario of the ejection of a BH from the companion galaxy. that was previously introduced by Haehneltetal.(2006). or Hoffman&Loeb(2007) and discussed in several following papers concerning HEO450-2958. such as Merrittetal.(2006) and Letaweetal.(2009). | The detection of a plausible host rules out the scenario of the ejection of a BH from the companion galaxy, that was previously introduced by \cite{haenelt} or \cite{hoffman07} and discussed in several following papers concerning HE0450-2958, such as \cite{merrit} and \cite{letg09}. |
. If the BH had been ejected with some gas to feed it. it would not be accompanied by a galaxy with stars. | If the BH had been ejected with some gas to feed it, it would not be accompanied by a galaxy with stars. |
The well-detected stellar emission from the blob sheds new light on recent attempts to explain this unusual system. | The well-detected stellar emission from the blob sheds new light on recent attempts to explain this unusual system. |
Indeed. Elbazetal.(2009) proposed that the activity of the quasar and associated radio jets have been creating the companion galaxy and parts of the host in construction. still partially disjoint from the QSO as seen in a primordial step of its evolution. | Indeed, \cite{elbaz} proposed that the activity of the quasar and associated radio jets have been creating the companion galaxy and parts of the host in construction, still partially disjoint from the QSO as seen in a primordial step of its evolution. |
The observation of stars in the direct vicinity of the QSO shows that there is already a host candidate. independently of the impact of the radio Jet on the surrounding objects. | The observation of stars in the direct vicinity of the QSO shows that there is already a host candidate, independently of the impact of the radio jet on the surrounding objects. |
Moreover. from the CO observations of Papadopoulosetal.(2008).. no star formation is found at the blob location. excluding the possibility that the QSO could have created the blob. | Moreover, from the CO observations of \cite{papad}, no star formation is found at the blob location, excluding the possibility that the QSO could have created the blob. |
These findings support the hypothesis already presented by Papadopoulosetal.(2008).. involving a collision between a gas rich galaxy (the companion). and a smaller one (the blob). | These findings support the hypothesis already presented by \cite{papad}, involving a collision between a gas rich galaxy (the companion), and a smaller one (the blob). |
Two galaxies have collided. each of them probably harbouring an active BH. the interaction enhancing the star formation in at least one of the galaxies and disrupting the pre-existing structures. | Two galaxies have collided, each of them probably harbouring an active BH, the interaction enhancing the star formation in at least one of the galaxies and disrupting the pre-existing structures. |
The disrupted parts will probably merge in the future into a single galaxy. | The disrupted parts will probably merge in the future into a single galaxy. |
The radio jet would play a secondary role in the enhancement of the star formation in some parts of the system ΠΠ the “tail” in between the main QSO and the companion galaxy. and maybe in the N-E part of the companion galaxy itself). | The radio jet would play a secondary role in the enhancement of the star formation in some parts of the system in the “tail" in between the main QSO and the companion galaxy, and maybe in the N-E part of the companion galaxy itself). |
Moreover. the QSO radiation would ionize the gas expelled all around the system (Letawe et al.. | Moreover, the QSO radiation would ionize the gas expelled all around the system (Letawe et al., |
2008b) In fact. this scenario explains all the observations: disturbed morphology in both galaxies (including off-centre nuclei). presence of the second AGN. enhanced star formation. N-E stellar emission and extended emission line regions. | 2008b) In fact, this scenario explains all the observations: disturbed morphology in both galaxies (including off-centre nuclei), presence of the second AGN, enhanced star formation, N-E stellar emission and extended emission line regions. |
The previous non detection ofthe stellar content in the blob was due to its faintness in the optical. its compactness and its proximity to the bright QSO. bringing the optical continuum just below the detection limits. | The previous non detection of the stellar content in the blob was due to its faintness in the optical, its compactness and its proximity to the bright QSO, bringing the optical continuum just below the detection limits. |
The secure detection of stars near the QSO. even if not centred on the nucleus. makes the HE0450-2958 system consistent with a highly perturbed merger. probably not requiring more exotic scenarios. | The secure detection of stars near the QSO, even if not centred on the nucleus, makes the HE0450-2958 system consistent with a highly perturbed merger, probably not requiring more exotic scenarios. |
As such. it fits reasonably well with the hierarchical models of galactic building by successive mergers. | As such, it fits reasonably well with the hierarchical models of galactic building by successive mergers. |
parallax analysis of absolute magnitude variations iu the AI dwarf population (Paper IT).. a detailed exauinatiou of M dwarf kinematics and the motions of the Galactic thin aud thick disks (Pinedaetal.2011.PaperΠΠ)... and an investigation of the content aud distribution of dust iu the local Claxy (Jonesetal.2011). | parallax analysis of absolute magnitude variations in the M dwarf population (Paper \nocite{boostat}, a detailed examination of M dwarf kinematics and the motions of the Galactic thin and thick disks \citep[Paper
III]{pineda10}, and an investigation of the content and distribution of dust in the local Galaxy \citep{jones11}. |
. In addition to the current and untorescen science that will be accomplished with our sample. we anticipate that our M. dwart catalog will be used to select aud classify M. dwarfs in. several upconius laree surveys. | In addition to the current and unforeseen science that will be accomplished with our sample, we anticipate that our M dwarf catalog will be used to select and classify M dwarfs in several upcoming large surveys. |
Over l1 billion M. dwarfs will be observed and cataloged in the new wave of large photometric survevs comme online in the next decade. | Over 1 billion M dwarfs will be observed and cataloged in the new wave of large photometric surveys coming online in the next decade. |
We hope that our large M. chwarf sample preseuted iu this paper will provide a useful tool for correlatiug the spectroscopic attributes of low-1ass stars with their photometric properties both iu single exposures aud im the time domain. | We hope that our large M dwarf sample presented in this paper will provide a useful tool for correlating the spectroscopic attributes of low-mass stars with their photometric properties both in single exposures and in the time domain. |
The authors would like to thauk Sebastian Léppine.5 Jackie Faherty. Adam Durgasser. Eveenva Shlikoluils and Edo Berger for useful discussions leading to the colmpletion of this catalog. | The authors would like to thank Sebastian Léppine, Jackie Faherty, Adam Burgasser, Evgenya Shkolnik and Edo Berger for useful discussions leading to the completion of this catalog. |
The authors also thank the anouvmous referee for his/her iusightful comuuents. which oereatle nmnuproved the quality of the original manuscript. | The authors also thank the anonymous referee for his/her insightful comments, which greatly improved the quality of the original manuscript. |
S.L.IT. aud J.J.D. ackuowledee the support of NSF AST eraut 06-0761L. | S.L.H. and J.J.B. acknowledge the support of NSF AST grant 06-07644. |
Π.Ο. acknowledges support for this work from the Iubble Fellowship Program. provided by NASA through Iubble Fellowship eraut HST-IIE-51253.01- awarded by the STScI. which is operated by the AURA. ÀInc.. for NASA. under contract NAS 5-26555. | K.R.C. acknowledges support for this work from the Hubble Fellowship Program, provided by NASA through Hubble Fellowship grant HST-HF-51253.01-A awarded by the STScI, which is operated by the AURA, Inc., for NASA, under contract NAS 5-26555. |
Funding for the Sloan Digital Skv Survey (SDSS) and SDSS-II has been provided bv the Alfred P. Sloan Foundation. the l'artiipatiue Tustitutions. the National Science. Foundation.ronauties the U.S. Department of Encrex. the National Acs aud Space Aciuinistration. the Japanese Moubukagakusho. aud the Max Planck Society. and the Iligher Education Funding Council for Euglaud. | Funding for the Sloan Digital Sky Survey (SDSS) and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, and the Max Planck Society, and the Higher Education Funding Council for England. |
The SDSS Wel site is http://vwiw.sdss.org/ The SDSS is managed by the Astrophysical Research Cousortimn ""(ARC) for the Participating Iustitutious. | The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. |
The Partic Tustitutions are the American Abuseun of Natural Iüstorv. Astrophysical Institute Potsdam. University of Basel. Uuiversitv of Cambridec. Case Western Reserve University. The University of Chicago. Drexel University. Fermilab. the Tustitute for Advanced Study. the Japan Participation Croup. The Johus IHopkius Umniversitv. the Joiut Institute for Nuclear Astrophysics. the Kavli Institute for Particle Astrophysics and Cosmology. the korean Scientist Caoup. the Chinese Academy of Sciences (LAMOST). Los Alamos National Laboratory. the Max- for Astrouauw (AIPIA). the Max-Plauck-Iustitute for Astrophysics (AIPA). New Mexico State University, Olio. State University. University of Pittsburgh. University. of Portsmouth. Princetou University. the United States Naval Observatory. aud the University of Washington. | The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, The University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. |
This publication makes use of data products from the Two Micron All Sky Survey. which is a joint project of the University of Massachusetts aud the Iufrared Processing and Analysis Center/California Institute of Technology. funded bv the National Aeronautics and Space Achuinistration and the National Science Foundation. | This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. |
afterglow flux level. | afterglow flux level. |
Results quoted in Tables 2,3 and 4 were obtained by extrapolating the X-ray afterglow at the three epochs where best optical/near-IR spectral coverage is available and by normalizing the best-fit temporal model obtained at optical wavelengths (?) at the X-ray unabsorbed flux value measured at T+3.254 days (Fig.1). | Results quoted in Tables 2,3 and 4 were obtained by extrapolating the X-ray afterglow at the three epochs where best optical/near-IR spectral coverage is available and by normalizing the best-fit temporal model obtained at optical wavelengths \citep{Tagliaferri2005} at the X-ray unabsorbed flux value measured at $T+3.254$ days (Fig.1). |
It may be argued that several GRBs show that X-ray and optical afterglow light curves do not decay with the same behavior (e.g.?).. | It may be argued that several GRBs show that X-ray and optical afterglow light curves do not decay with the same behavior \citep[e.g.][]{Panaitescu2006}. |
However, even though there is also a non negligible fraction of GRBs for which the optical and X-ray emission decay jointly (e.g.?),, GRB 050904 is one of the few bursts for which a broad band modeling was feasible from radio to X-rays. | However, even though there is also a non negligible fraction of GRBs for which the optical and X-ray emission decay jointly \citep[e.g.][]{Oates2011}, GRB 050904 is one of the few bursts for which a broad band modeling was feasible from radio to X-rays. |
In particular, it has been found that data are generally consistent with fireball paradigms, with the synchrotron cooling frequency below the optical range at the epochs of interest, thus supporting our assumption (e.g.?).. | In particular, it has been found that data are generally consistent with fireball paradigms, with the synchrotron cooling frequency below the optical range at the epochs of interest, thus supporting our assumption \citep[e.g.][]{Frail2006}. |
In addition, results for dust extinction at T+0.47 and T+1.25 days are on average consistent with the A3zo99 values obtained at T+3.4 days, when the Swift/XRT observations are available at T+3.254 days, and thus flux extrapolation depends little on the assumed temporal model. | In addition, results for dust extinction at $T+0.47$ and $T+1.25$ days are on average consistent with the $A_{3000}$ values obtained at $T+3.4$ days, when the Swift/XRT observations are available at $T+3.254$ days, and thus flux extrapolation depends little on the assumed temporal model. |
At T+3.4 days, the extracted X-ray to optical SED shows clear evidence of dust extinction, with Asooo in the range that goes from 0.2 to 0.9 mag, depending on the assumed dust recipe (Tab. | At $T+3.4$ days, the extracted X-ray to optical SED shows clear evidence of dust extinction, with $A_{3000}$ in the range that goes from 0.2 to 0.9 mag, depending on the assumed dust recipe (Tab. |
4). | 4). |
These results indicate, beyond a doubt, that the primeval galaxy at z=6.3 hosting this GRB has already enriched its ISM with dust. | These results indicate, beyond a doubt, that the primeval galaxy at z=6.3 hosting this GRB has already enriched its ISM with dust. |
However, while the presence of dust attenuating the GRB 050904 optical afterglow at any epoch is firmly established, the type of extinction/attenuation curve is not well constrained, although we find that only the SMC and SN-type extinction curves provide a good fit to the data 68%)) at all epochs (Fig. | However, while the presence of dust attenuating the GRB 050904 optical afterglow at any epoch is firmly established, the type of extinction/attenuation curve is not well constrained, although we find that only the SMC and SN-type extinction curves provide a good fit to the data $P(\tilde{\chi}^2<\tilde{\chi}^2_{BF})<68$ ) at all epochs (Fig. |
2). | 2). |
We reanalyzed the afterglow of GRB 050904 at z=6.3 at those epochs where the best spectral coverage is available in the optical/near-IR range (UV rest frame), namely at 0.47, 1.25, and 3.4 days after the trigger, by fitting the simultaneous optical/near-IR and X-ray SED. | We reanalyzed the afterglow of GRB 050904 at z=6.3 at those epochs where the best spectral coverage is available in the optical/near-IR range (UV rest frame), namely at 0.47, 1.25, and 3.4 days after the trigger, by fitting the simultaneous optical/near-IR and X-ray SED. |
In this work, we exploited the recent reanalysis done by ? on Z-band data, which are the most sensitive to dust reddening for this burst. | In this work, we exploited the recent reanalysis done by \cite{Zafar2010} on Z-band data, which are the most sensitive to dust reddening for this burst. |
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