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A nore physically mcaninefil tcst is whether E.this correlated with the rest-frame duralon. Zo9/(1|2). | A more physically meaningful test is whether $E_{\gamma,{\rm iso}}$ is correlated with the rest-frame duration, $T_{90}/(1+z)$. |
Iu case. I fiud that for the cight bursswith secure redshifts the null. hypothesis ji a probabiitv of L5«103. sO zu overall correlation docs lot apear to be statistically meaninefil. | In this case, I find that for the eight bursts with secure redshifts the null hypothesis has a probability of $4.5\times 10^{-2}$, so an overall correlation does not appear to be statistically meaningful. |
Curiously. the sample «six bursts witli secure redshifts and late-ty25 host eaaxies has p=0.91 (null hypothesis probabiliv of oulv 6\1j Hd mt this result is likely due to siiall iimiber statistic‘ss. | Curiously, the sample of six bursts with secure redshifts and late-type host galaxies has $\rho=0.94$ (null hypothesis probability of only $6\times 10^{-4}$ ), but this result is likely due to small number statistics. |
To coucludoe. there is sole tentative evideice for a positive correlation between enerev release and duration. but tus will have to be assessed With a larger sample. | To conclude, there is some tentative evidence for a positive correlation between energy release and duration, but this will have to be re-assessed with a larger sample. |
Suuilulv. I check or a relation betwee1 ΟΗΟΥΟΥ release and host ealaxy type. | Similarly, I check for a relation between energy release and host galaxy type. |
This is the case for Type la supernovae (SNe Ia). which tend to have lower Iuuiuosities in carly-type eaaxies than in late-type eaaxies. likely due o a dependence on the progenitor ages (Gallagheretal.2005:Sullivanetal. 2006). | This is the case for Type Ia supernovae (SNe Ia), which tend to have lower luminosities in early-type galaxies than in late-type galaxies, likely due to a dependence on the progenitor ages \citep{ggb+05,slp+06}. |
. Short CRBs also occur in both vpes of galaxies so a similar trend iav shed light on the xogenuitor properties. | Short GRBs also occur in both types of galaxies so a similar trend may shed light on the progenitor properties. |
In the sample prescuted here. three mrsts have hee1 localized to early-type galaxies (050509). 15072 Land 050813). while six lave| Secure late-type hosts (050709. 051221a. 0608501. 061006 061210. aud. 061217). | In the sample presented here, three bursts have been localized to early-type galaxies (050509b, 050724, and 050813), while six have secure late-type hosts (050709, 051221a, 060801, 061006, 061210, and 061217). |
As can be seen from Table1. both eroups appear to span he full range of -rav energies and X-ray hDpuuuinosities. sugecsting no clear correlation with host ealaxy type for he present sample. | As can be seen from Table \ref{tab:data} both groups appear to span the full range of $\gamma$ -ray energies and X-ray luminosities, suggesting no clear correlation with host galaxy type for the present sample. |
Finally. Ireturn to t1e 20% of outliers with an uuustally low ratio of Fy4fEF... | Finally, I return to the $20\%$ of outliers with an unusually low ratio of $F_{X,1}/F_\gamma$. |
The possible nature of these objects has been discussed. 1 Nakar(200T) who noted several possibilities for the suopressed X-ray flux. im particular a low circtuuburst density (09<LOD cm 3), typical of the interealactic medina. | The possible nature of these objects has been discussed by \citet{nak07} who noted several possibilities for the suppressed X-ray flux, in particular a low circumburst density $n\lesssim 10^{-5}$ $^{-3}$ ), typical of the intergalactic medium. |
This is argue Lto support the idea of large kick velocities. >107 Iain Ἐν for some progeniOr. | This is argued to support the idea of large kick velocities, $\gtrsim
10^2$ km $^{-1}$, for some progenitors. |
Tere E simply note that while all fo1 routliers have fiueuces at the low eud of the distribution. F.oxOd0* ore ? (Figure 1)). the two wit1 redslüft constraints (t50813 aud 051210) appear to reside at 2m1.5 aud therefore their energies are at the hieh end of the «overall distributiou. | Here I simply note that while all four outliers have fluences at the low end of the distribution, $F_\gamma\lesssim 10^{-7}$ erg $^{-2}$ (Figure \ref{fig:fxfgamma}) ), the two with redshift constraints (050813 and 051210) appear to reside at $z\gtrsim 1.5$ and therefore their energies are at the high end of the overall distribution. |
No other parameters clearly distinguis ithe outliers from the mul of the population that has a narrow distribution of e.. sneeestingOO that indeed an extiasic piarsuueter such as he density is responsible for their ow N-rav fluxes. | No other parameters clearly distinguish the outliers from the bulk of the population that has a narrow distribution of $\epsilon_\gamma$, suggesting that indeed an extrinsic parameter such as the density is responsible for their low X-ray fluxes. |
Iu the coutext of a low density 1iterpretation for these outlicrs. and eiveu the clearly bimodal distribution. I xopose the following intriguing possibility. | In the context of a low density interpretation for these outliers, and given the clearly bimodal distribution, I propose the following intriguing possibility. |
The observed yaction of is simular to predictions of the fraclon of short CRBs that iav arise from dviiuuicallv-forned jicutron star binaries in elobular clusters (1030| Caindlayetal. 2006)). | The observed fraction of is similar to predictions of the fraction of short GRBs that may arise from dynamically-formed neutron star binaries in globular clusters $10-30\%$; \citealt{gpm06}) ). |
This scenaric» nay naturally explain he required low censitics since tlic! jutra-cluster medina of elobular clusters has a typical of n<few10 5m (vanLoonetal.2006).. likely as a result of eas stripping from frequent passages twouel tje Galactic disk. | This scenario may naturally explain the required low densities since the intra-cluster medium of globular clusters has a typical of $n\lesssim {\rm few}\times 10^{-5}$ $^{-3}$ \citep{lse+06}, likely as a result of gas stripping from frequent passages through the Galactic disk. |
This scenario aso naturally explains the bimodal distribution of FyfF. (aud heuce densities). siice the bursts occur iu either interstellar euviromnuents wiμη x050a 7 rofsec:iepsilou)) or in the low ce‘sity environments of elobular clusters. | This scenario also naturally explains the bimodal distribution of $F_X/F_\gamma$ (and hence densities), since the bursts occur in either interstellar environments with $n\gtrsim 0.05$ $^{-3}$ \\ref{sec:epsilon}) ) or in the low density environments of globular clusters. |
Thus. fus alternative scenario renioves the need for speculative large kick velocities for the outlicrs Nalkar2007).. which i) uy case prediets a muore παον distribution of densitiesμα aud hence PyfF. than currently observed. | Thus, this alternative scenario removes the need for speculative large kick velocities for the outliers \citep{nak07}, which in any case predicts a more uniform distribution of densities and hence $F_X/F_\gamma$ than currently observed. |
Based on proiip -Yav aud N-ray afterelow observations of a sample of 17 short GRBs with rapid NRT follow-up I find the following results: With hese properties of short CRBs well-established the next step is fo assess the iuportance of beanuue corrections. and lence the true distribution of total relativistic οἱtput from the centra engenie. | Based on prompt $\gamma$ -ray and X-ray afterglow observations of a sample of 17 short GRBs with rapid XRT follow-up I find the following results: With these properties of short GRBs well-established the next step is to assess the importance of beaming corrections, and hence the true distribution of total relativistic output from the central engine. |
I thank Alicia Soderberg aud E πια>Nakar for valuable ciseussion. aid acknowledge support|w NASA through IIubble Fellowship eraut IIST-01]Tl.Ol awarded by the Space Tele MUNScience Institute. which is operated by AURA. Inc. for NASA under coutract NAS 5-2655h, | I thank Alicia Soderberg and Ehud Nakar for valuable discussion, and acknowledge support by NASA through Hubble Fellowship grant HST-01171.01 awarded by the Space Telescope Science Institute, which is operated by AURA, Inc. for NASA under contract NAS 5-26555. |
stellar parameters. | stellar parameters. |
By defining aas (lie energy integral of ἐπ...7x) above the eedge (erg em7s +). then our fundamental adjustable parameter used in this study is defined as where F, is the total stellar photospherie flux. μιἐπη,)]. | By defining as the energy integral of $4 \pi \JX(E,\TX)$ above the edge (erg $^{-2}$ $^{-1}$ ), then our fundamental adjustable parameter used in this study is defined as where $F_*$ is the total stellar photospheric flux $\Lbol / 4 \pi \Rstar^2$ ). |
Uence. for a given. F,.FE. and Ty... ccan be extracted directly from where A(ZX) (erg cms +) is the total energy integral of 4xe(E.TX) above the eedee. | Hence, for a given $F_*$, and , can be extracted directly from where $\Lambda (\TX)$ (erg $^3$ $^{-1}$ ) is the total energy integral of $4 \pi \epsilon (E, \TX)$ above the edge. |
Note (hat iis not (he same as (he well known observed X-ray to bolometric luminosity ratio.Lj.. because in (his ralio is an "observed quantity. ie... a measure of only those X-rays capable of escaping the stellar wind. aud our iis defined as an intrinsic total mean intensitv (Gin flux units) where the majority of this emission (i.e.. NUV) resides in an observational window that is inaccessible cue to wind and ISAT attenuation. | Note that is not the same as the well known observed X-ray to bolometric luminosity ratio, because in this ratio is an “observed” quantity, i.e., a measure of only those X-rays capable of escaping the stellar wind, and our is defined as an intrinsic total mean intensity (in flux units) where the majority of this emission (i.e., XUV) resides in an observational window that is inaccessible due to wind and ISM attenuation. |
The predicted ddependence on [for supergiants. giants. and main sequence stars is shown in Figure 4. | The predicted dependence on for supergiants, giants, and main sequence stars is shown in Figure 4. |
Also shown in this Figure are the data points [rom FOG that correspond to the required vvalues if all stus have their traditional wwhich we will use to determine the constraints on/F. | Also shown in this Figure are the data points from F06 that correspond to the required values if all stars have their traditional which we will use to determine the constraints on. |
.. This deficit in rrelative to unity led FOG to conclude that nneeds (o be reduced. | This deficit in relative to unity led F06 to conclude that needs to be reduced. |
Figure 4 shows a strong dependence of oon/F,.. aud indicates that a range in bbetween (0.3—10)x10* can explain the observed [for all luminosity classes. | Figure 4 shows a strong dependence of on, and indicates that a range in between $(0.3 ~ - ~ 10) \times 10^{-7}$ can explain the observed for all luminosity classes. |
For example. [rom Figure 4. (he observed ool the four supergiants at 7;;;=35000 indicate a Fy/F,22.5x10*. | For example, from Figure 4, the observed of the four supergiants at $\Teff = 35000$ indicate a $\FXFS \approx 2.5 \times 10^{-7}$. |
This implies a χιΧαν flux z2x10* erg 7s banda zz2.5x107" em (using Eq. | This implies a XUV+X-ray flux $ \approx 2 \times 10^{7}$ erg $^{-2}$ $^{-1}$ and a $\approx 2.5 \times 10^{29}$ $^{-5}$ (using Eq. |
D). | 1). |
From X-ray analyses of OB stars we cannot directly determine ssince only the volume emission measure FAL, 7) can be deduced [rom observations. | From X-ray analyses of OB stars we cannot directly determine since only the volume emission measure $EM_V$ $^{-3}$ ) can be deduced from observations. |
If we assume that the NUV-EX-ray. radiation arises from a spherically shell at (he assumed | If we assume that the XUV+X-ray radiation arises from a spherically shell at the assumed |
ACXGN's whose substantial brightness means that more than a century of optical observations are available (c.e.. Carini et 11992b: Sillanpáà et 11996a. 1996h: Fn et 22002. 2009: Abraham et 0: Gupta et aL22008c). | AGN's whose substantial brightness means that more than a century of optical observations are available (e.g., Carini et 1992b; Sillanpää et 1996a, 1996b; Fan et 2002, 2009; Abraham et 2000; Gupta et 2008c). |
Using binary black hole model (Sillanpaa et 11988) for 1e long-term optical light curve of the source. an outburst with a predicted 12 vear period was detected in the source w the OJ-94 programme (Sillanpaa et al. | Using the binary black hole model (Sillanpää et 1988) for the long-term optical light curve of the source, an outburst with a predicted $\sim$ 12 year period was detected in the source by the OJ-94 programme (Sillanpää et al. |
1996a: Valtonen et 22008). | 1996a; Valtonen et 2008). |
On re-analvsing the optical data from O.J-94 project. Wu et ((2006) reported another possible iniescale. sugeesting a periodicity of ~40 cays. | On re-analysing the optical data from OJ-94 project, Wu et (2006) reported another possible timescale, suggesting a periodicity of $\sim$ 40 days. |
Very. high optical polarization that is variable in both degree and angle ias been reported in the source (IZlimov ct 22002). | Very high optical polarization that is variable in both degree and angle has been reported in the source (Efimov et 2002). |
The observational properties of OJ 287 [rom radio to X-ray enerev bands have been reviewed by TFakalo et ((1994). | The observational properties of OJ 287 from radio to X-ray energy bands have been reviewed by Takalo et (1994). |
During their observations spanning 2002 to 2007 Fan et (2009). reported large variations in the source of AV = 1.96 mag. AR = 2.36 mag. and Al = 1.95 mae. | During their observations spanning 2002 to 2007 Fan et (2009), reported large variations in the source of $\Delta$ V = 1.96 mag, $\Delta$ R = 2.36 mag, and $\Delta$ I = 1.95 mag. |
We found O.] 287 to have significant [ux variations in all 16 observed. passbands but no significant colour variation was found 66) | We found OJ 287 to have significant flux variations in all the observed passbands but no significant colour variation was found 6). |
A [lare in the LCS of the blazar Οἱ) 287 οἱ —1L mag was observed in all bands over an interval of 36 claws. but we had only one night. of data near the Ilare's peak so it is quite likely that the maximum of the Hare was even stronger. | A flare in the LCs of the blazar OJ 287 of $\sim$ 1 mag was observed in all bands over an interval of 36 days, but we had only one night of data near the flare's peak so it is quite likely that the maximum of the flare was even stronger. |
Lt is interesting that this result is consistent with a ~37 day period of rotation of the the plane of polarization seen of OJ 287 (Efimovy ct 22002) and close to a 40 day periodicity reported in source by Wu et ((2006). | It is interesting that this result is consistent with a $\sim$ 37 day period of rotation of the the plane of polarization seen of OJ 287 (Efimov et 2002) and close to a 40 day periodicity reported in source by Wu et (2006). |
The average It band magnitude (1t ~ 14.7 mag) of the source curing our run is ~2.5 mag [nter than the brightest (I5— 12.O imag) civisand 72.3 magnitude brighter than the faintest magnit (1t — 16.47 mag) reported in the source bv Fan et ((2000). | The average R band magnitude (R $\sim$ 14.7 mag) of the source during our observing run is $\sim$ 2.5 mag fainter than the brightest (R = 12.09 mag) and $\sim$ 2.3 magnitude brighter than the faintest magnitude (R = 16.47 mag) reported in the source by Fan et (2000). |
So it seems that we observed ©.) 287 in an intermediate state. | So it seems that we observed OJ 287 in an intermediate state. |
This optically violent variable quasar belongs o the class of FSROQs. | This optically violent variable quasar belongs to the class of FSRQs. |
At both optical and LR bands STV and LEV have been observed in this source (Branly ct 11996: Noble Miller 1996: Chosh ct 22000). | At both optical and IR bands STV and LTV have been observed in this source (Branly et 1996; Noble Miller 1996; Ghosh et 2000). |
A very arge variation (AV 7 5 mag) has been reported in the source during the optical outburst of. 1981. (Wills et. 11983). | A very large variation $\Delta$ V $>$ 5 mag) has been reported in the source during the optical outburst of 1981 (Wills et 1983). |
Large fractional polarizations. up to —28'A. have xen observed in 4€ 29.45 both at optical and LR. frequencies (Llolmes et 14984: Mead et 11990) | Large fractional polarizations, up to $\sim$ $\%$, have been observed in 4C 29.45 both at optical and IR frequencies (Holmes et 1984; Mead et 1990). |
ες optical [Dux and colour variations have been recently studied by Fan et ((2006). | Its optical flux and colour variations have been recently studied by Fan et (2006). |
They have reported amplitude variations of ~4.5 6 mag in all passbands (U. D. V. It. D) anc also found that here were possible periods of 3.55 or 1.58 vears in the long erm optical light curve of the source. | They have reported amplitude variations of $\sim$ 4.5 – 6 mag in all passbands (U, B, V, R, I) and also found that there were possible periods of 3.55 or 1.58 years in the long term optical light curve of the source. |
Our LCs of 4€ 29.45 indicate that it is variable in all he observed. bands but the percentage of variation cillers substantially among them. leading to the significant colour variations 77). | Our LCs of 4C 29.45 indicate that it is variable in all the observed bands but the percentage of variation differs substantially among them, leading to the significant colour variations 7). |
During our observing run 4€ 29.45 varied from (Fig.16.30 to 17.57. magnitude in the | band. | During our observing run 4C 29.45 varied from 16.30 to 17.57 magnitude in the I band. |
The faintest magnitude we observed in the source is thus 0.12 magnitudes fainter that the faintest level. b= 17.45+0.05 mag. reported. for this source by Fan ct ((2006) so we clearly observed the source in a faint phase. | The faintest magnitude we observed in the source is thus 0.12 magnitudes fainter that the faintest level, I = $\pm$ 0.05 mag, reported for this source by Fan et (2006) so we clearly observed the source in a faint phase. |
The faintest state of the source was on 23 May 2009 but it had brightened by ~0.2 mag by the next day. | The faintest state of the source was on 23 May 2009 but it had brightened by $\sim$ 0.2 mag by the next day. |
The FSRQ 3€ 273 was the first quasar discovered (Schmidt. L963). | The FSRQ 3C 273 was the first quasar discovered (Schmidt 1963). |
Categorized as a LBL (Nicppola ct 22006). its spectral energy. distribution. correlations among ares in different energy. bands and the approaching jet's orientation have been extensively studied at all LAL bancs (e.g. Valtaoja et 11991b: Takalo et 11992a. 1992). | Categorized as a LBL (Nieppola et 2006), its spectral energy distribution, correlations among flares in different energy bands and the approaching jet's orientation have been extensively studied at all EM bands (e.g., Valtaoja et 1991b; Takalo et 1992a, 1992b). |
Many papers cover ὃς 23s observational properties of the source in the visible band (CXngione et 11981: Sitko ct 11982: Corso ct 11985. 1986: Moles et al. | Many papers cover 3C 273's observational properties of the source in the visible band (Angione et 1981; Sitko et 1982; Corso et 1985, 1986; Moles et al. |
1986: Llaniuy Maza 1987: Sillanpaad et al. | 1986; Hamuy Maza 1987; Sillanpää et al. |
1991: Valtaoja et al. | 1991; Valtaoja et al. |
1991b: ‘Takalo ct al. | 1991b; Takalo et al. |
19922. PM Elvis ct MN Lichti ct al. | 1992a, 1992b; Elvis et 1994; Lichti et al. |
1995: CGhosh et 22000:M Dai et d | 1995; Ghosh et 2000; Dai et 2005). |
of the optical light. curve 3C 273 pannis overOn LOOn vears suggests a LEV timescale of ~13.5 vears (Fan. ‘Tao 2001). | Analyses of the optical light curve of 3C 273 spanning over 100 years suggests a LTV timescale of $\sim$ 13.5 years (Fan, Qian Tao 2001). |
Recenth. the SLY and colour index properties of the source were studied by Dai οἱ ((2009). | Recently, the STV and colour index properties of the source were studied by Dai et (2009). |
They. found a strong correlation between the colour index and. brightness of the source in the sense that the spectrum becomes Latter, or bluer. when the source brightens and steeper. or reddoer. when it [acles. | They found a strong correlation between the colour index and brightness of the source in the sense that the spectrum becomes flatter, or bluer, when the source brightens and steeper, or redder, when it fades. |
The blazar 3C 273 was essentially in a steady state during our observing run. with no significant variation ereater than —0.03 mag in anv of the observed. LCs SS). | The blazar 3C 273 was essentially in a steady state during our observing run, with no significant variation greater than $\sim$ 0.03 mag in any of the observed LCs 8). |
Nor were any significant variations found in the colour LCs of the source. | Nor were any significant variations found in the colour LCs of the source. |
Very recently. Dai et ((2009) reported that the source also was essentially steady curing their observations. which ran from January 2003 to April 2005 ih an average 1t band magnitude 212.44 which was only "A12 mag brighter than that of our observing run (lt = 2.56 mag). | Very recently Dai et (2009) reported that the source also was essentially steady during their observations, which ran from January 2003 to April 2005, with an average R band magnitude $\simeq$ 12.44 which was only 0.12 mag brighter than that of our observing run (R = 12.56 mag). |
Thus it is very n that the same dull state continued in 3€ 273 (rom 2063 through our observations in 2009. | Thus it is very possible that the same dull state continued in 3C 273 from 2003 through our observations in 2009. |
This PSRQ and shows strong optical polarization and [lux variabilities at all. frequencies. | This FSRQ and shows strong optical polarization and flux variabilities at all frequencies. |
X very large amplitude. variation of AB 6.7 in the optical Dux of 3€ 279 was reported long ago by Eachus Liller (1975). | A very large amplitude variation of $\Delta$ B $\geq$ 6.7 in the optical flux of 3C 279 was reported long ago by Eachus Liller (1975). |
A rapid variation of 1.17 mag within 40 minutes was seen in the V band (Xie et 11999) and a STV of 0.91 mag in the It. band. was seen over 49 days (Xie et 220025). | A rapid variation of 1.17 mag within 40 minutes was seen in the V band (Xie et 1999) and a STV of 0.91 mag in the R band was seen over 49 days (Xie et 2002b). |
Recently. Gupta οἱ en2008c) reported a 1.5 mag variation in the It. band. of 3¢ over 42 clavs but Webb ct ((1990) reported rapid. Huctuations of ~2 mag within 24 hours at. visible wavelengths. | Recently, Gupta et (2008c) reported a 1.5 mag variation in the R band of 3C 279 over 42 days but Webb et (1990) reported rapid fluctuations of $\sim$ 2 mag within 24 hours at visible wavelengths. |
Not surprisingly. this source also has been intensively studied through multi-wavelength campaigns (Llartman et 119t1G: Welle et al. | Not surprisingly, this source also has been intensively studied through multi-wavelength campaigns (Hartman et 1996; Wehrle et al. |
1998). | 1998). |
The most recent. WEBT campaign on 3€ 279 reported that the source was in the high optical state and the LCs show exponential decavs of llux of —1 mag on a time scale of ]2.8 davs (Botttcher et al. | The most recent WEBT campaign on 3C 279 reported that the source was in the high optical state and the LCs show quasi-exponential decays of flux of $\sim$ 1 mag on a time scale of $\sim$ 12.8 days (Bötttcher et al. |
2007) which was explained by Bottteher Principe (2009) as a signature of deceleration of a svynchrotron emitting jet component. | 2007) which was explained by Bötttcher Principe (2009) as a signature of deceleration of a synchrotron emitting jet component. |
]t is clear from our LCSs that the source is highly variable in all the observed passbands 99). | It is clear from our LCs that the source is highly variable in all the observed passbands 9). |
However. except for L the colours of the source are not significantly variable. | However, except for $-$ I. the colours of the source are not significantly variable. |
3C 27098 LC shows a rapid decay in brightness. Le... within 5 davs AV = 124 mag. AR = 1.10 mag ancl Al mag which is faster than most earlier S'TVs reported in the source (e.g... Xie et 220 er3ottteher et 22007: Xie et 11999: Ciupta et 22008Ts | 3C 279's LC shows a rapid decay in brightness, i.e., within 5 days $\Delta$ V = 1.24 mag, $\Delta$ R = 1.10 mag and $\Delta$ I = 0.8 mag which is faster than most earlier STVs reported in the source (e.g., Xie et 2002b; Bötttcher et 2007; Xie et 1999; Gupta et 2008c). |
Cups~The source was reported to be in outburst in Jan20 et .((2008c€)vel reaching a brightness of It —12.6 mag. | The source was reported to be in outburst in Jan 2007 by Gupta et (2008c) reaching a brightness of R $\sim$ 12.6 mag. |
The faintest we observed for 3€ 279 was lt — 17.1 mag which is ~4.5 magnitudes fainter than the outburst brightness seen about 24 vears earlier. indicating that we caught 3€ ) classifiedin à low-state. | The faintest level we observed for 3C 279 was R = 17.1 mag which is $\sim$ 4.5 magnitudes fainter than the outburst brightness seen about 2.4 years earlier, indicating that we caught 3C 279 in a low-state. |
This source is as a ESBRO and | This source is classified as a FSRQ and |
mani. | maximum. |
The main quantitative results of this investigation are contained in Figure 5 ancl Table 3. | The main quantitative results of this investigation are contained in Figure 5 and Table 3. |
What follows is a proposed physical framework which could accommodate the chemical evolution scenario described above. | What follows is a proposed $physical$ framework which could accommodate the chemical evolution scenario described above. |
Basically. we envision (he anisotropic collapse of a number of initially isolated. cuiescently evolving. protogalactic clumps. | Basically, we envision the anisotropic collapse of a number of initially isolated, quiescently evolving, protogalactic clumps. |
The initial configuration is {hen either a (riaxial halo (CDM) or a fragmented sheet or flattened filament (WDAI). | The initial configuration is then either a triaxial halo (CDM) or a fragmented sheet or flattened filament (WDM). |
Evidence which supports these initial conditions is (he triaxial spatial distribution of the oullving satellites of the Galaxy. (lartwick 2000) along with a similar alignment of the space distribution and space motions of the blue elobular clusters (Hartwick 2002). | Evidence which supports these initial conditions is the triaxial spatial distribution of the outlying satellites of the Galaxy (Hartwick 2000) along with a similar alignment of the space distribution and space motions of the blue globular clusters (Hartwick 2002). |
During the first collapse. which is (ransverse to the long (rotation) axis. the low angular momentum chimps will collide to form the blue globular clusters. | During the first collapse, which is $transverse$ to the long (rotation) axis, the low angular momentum clumps will collide to form the blue globular clusters. |
In turn. the gas released in the collisions will fall towards the center to form the bulge. | In turn, the gas released in the collisions will fall towards the center to form the bulge. |
Support for a low angular momentum halo-bulge connection can be found in the review of Wyse et ((1997). who show (their Figure 7) that the distribution of the specific angular momentum of the (classical) halo and bulge are similar and unlike the disk/thick disk distribution. | Support for a low angular momentum halo-bulge connection can be found in the review of Wyse et (1997), who show (their Figure 7) that the distribution of the specific angular momentum of the (classical) halo and bulge are similar and unlike the disk/thick disk distribution. |
The higher angular momentum chimps will generally not collide initially. but insteac will fall towards the center along the long axis while still forming stars and enriching the gas within them. | The higher angular momentum clumps will generally not collide initially, but instead will fall towards the center along the long axis while still forming stars and enriching the gas within them. |
These clumps will eventually meet at what will become the plane of the disk. | These clumps will eventually meet at what will become the plane of the disk. |
ed clusters then form in these collisions. and (he gas released settles down to form the disk. | Red clusters then form in these collisions, and the gas released settles down to form the disk. |
The stars which had previously formed continue their dvnamical evolution back out into the halo. | The stars which had previously formed continue their dynamical evolution back out into the halo. |
The MDE of this group of stars should be similar to the dashed. curve in Figure 2. with a peak at [Fe/II]o—0.8 and with an angular momentum distribution like (he (hin disk. | The MDF of this group of stars should be similar to the dashed curve in Figure 2, with a peak at $
\sim-0.8$ and with an angular momentum distribution like the thin disk. |
Note that there is a metal poor tail associated with this MDE. | Note that there is a metal poor tail associated with this MDF. |
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