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. Lt provides simultaneous. sine-wave fitting and. least-squares fitting algorithms. | It provides simultaneous sine-wave fitting and least-squares fitting algorithms. |
The results were thereafter cross-checked with an analysis performed with the iterative sine-wave fitting method 1971) and found to agree within the The spectral window of the data shows the typical features of high precision satellite data: alias peaks have low amplitudes (smaller than 0.1 normalized. amplitucte. see upper panel of Fig. 3)) | The results were thereafter cross-checked with an analysis performed with the iterative sine-wave fitting method \citep{van71} and found to agree within the The spectral window of the data shows the typical features of high precision satellite data: alias peaks have low amplitudes (smaller than 0.1 normalized amplitude, see upper panel of Fig. \ref{prewhitening}) ) |
and are centered. around the orbital [reeueney and its multiplets. | and are centered around the orbital frequency and its multiplets. |
Phe orbital period of ColtoT is 6184 s CXuvergneetal.2009)).. corresponding toa frequency of fi,=13.97 dt. | The orbital period of CoRoT is 6184 s \citep{auv}, , corresponding to a frequency of $f_{orb} = 13.97$ $^{-1}$. |
In addition to the fur. we also find the term 2f;=2.0054 1. which is caused by the two passages over the South Atlantic Anomaly per day. and its harmonic Εως | In addition to the $f_{orb}$ we also find the term $2f_{sid} = 2.0054$ $^{-1}$, which is caused by the two passages over the South Atlantic Anomaly per day, and its harmonic $4f_{sid}$. |
Phe term fcr=1.0027 α itself is not visible in the spectral window. but its combinations with fi, are present. | The term $f_{sid}=1.0027$ $^{-1}$ itself is not visible in the spectral window, but its combinations with $f_{orb}$ are present. |
In summary. we find peaks at with O<&x6 and Ὁx7. | In summary, we find peaks at with $0 \leq k \leq 6$ and $1 \leq n \leq 7$. |
The highest peaks are at (hon)=(1.1). (k.n) = (2.0) and (k.n) = (0.2). | The highest peaks are at $(k,n) = (1,\pm1)$, (k,n) = (2,0) and (k,n) = (0,2). |
The dominant features in the Fourier spectrum of CoRoT 105288363 are the radial fundamental pulsation requeney of 17622967 cot and its numerous harmonics describing. the asymmetric light curve. shape that. is vpical for Rab stars. | The dominant features in the Fourier spectrum of CoRoT 105288363 are the radial fundamental pulsation frequency of 1.7622967 $^{-1}$ and its numerous harmonics describing the asymmetric light curve shape that is typical for RRab stars. |
Phe harmonics were significant up to the 22ncl order. when applying a significance criterion of a signal-to-noise ratio of 3.5 for combination requencics. | The harmonics were significant up to the 22nd order, when applying a significance criterion of a signal-to-noise ratio of 3.5 for combination frequencies. |
The noise amplitude calculated in the 2-12 d | range is 0.07 mimag and. is probably still alfected » the long-term instrumental drift. | The noise amplitude calculated in the 2-12 d $^{-1}$ range is 0.07 mmag and is probably still affected by the long-term instrumental drift. |
Indeed. it is lower (0.04 mmag) in the 50-90 * region. | Indeed, it is lower (0.04 mmag) in the 50-90 $^{-1}$ region. |
The well-known riplet structure with a spacing of the Blazhko frequency (in this case 0.028 i ) that is usually observed. in Blazhko stars. is also clearly visible. | The well-known triplet structure with a spacing of the Blazhko frequency (in this case 0.028 $^{-1}$ ) that is usually observed in Blazhko stars, is also clearly visible. |
The triplet. could either be caused by a nonradial mode close to the main »ulsation mode and its many combinations (Dreger&Ixolenberg||. 2006).. or it. could. simply result. from the modulation of purcly radial pulsation as was recently mathematically described by Szeicl&Jurseik(2009) and. using a cdillerent approach. hy Benksetal.(2009). | The triplet could either be caused by a nonradial mode close to the main pulsation mode and its many combinations \citep{bre06}, or it could simply result from the modulation of purely radial pulsation as was recently mathematically described by \citet{szei} and, using a different approach, by \citet{ben09}. |
The micelle panels of Fig. | The middle panels of Fig. |
3. show the Fourier spectrum of the original data. after subtraction of fy and its first 9 harmonics and alter subtraction of a fit including the triplet’ components. respectively. | \ref{prewhitening} show the Fourier spectrum of the original data, after subtraction of $f_0$ and its first 9 harmonics and after subtraction of a fit including the triplet components, respectively. |
Inserts show a zoom. into the vicinity of the 4th harmonic to illustrate the line structure of the remaining The ephemoerides of maximum pulsation light and maxiniun pulsation amplitude (Le. Blazhko maximum) found from. a classical Fourier analysis of the complete data set are: Note that as the Blazhko οσοι undergoes strong changes in CoRoT 105288363 (as can already be guessed after a close. inspection of the raw data shown in Figure 1)). | Inserts show a zoom into the vicinity of the 4th harmonic to illustrate the fine structure of the remaining The ephemerides of maximum pulsation light and maximum pulsation amplitude (i.e., Blazhko maximum) found from a classical Fourier analysis of the complete data set are: Note that as the Blazhko effect undergoes strong changes in CoRoT 105288363 (as can already be guessed after a close inspection of the raw data shown in Figure \ref{lightcurve}) ). |
Llenee the values above should beunderstood as mean values of the complete data set. | Hence the values above should beunderstood as mean values of the complete data set. |
A detailed investigation of the DBlazhko period. and changes of the Blazhko effect. using different approaches will be | A detailed investigation of the Blazhko period and changes of the Blazhko effect using different approaches will be |
In Paper I we sought a variety of evidence for the cause of the variability of the bright northern star 9 Aurigae. | In Paper I we sought a variety of evidence for the cause of the variability of the bright northern star 9 Aurigae. |
From UINIICE. LRAS. IUIS. and speckle data. it showed no evidence for a close companion or an orbiting lumpy ring of dust. ( | From UKIRT, IRAS, IUE, and speckle data, it showed no evidence for a close companion or an orbiting lumpy ring of dust. ( |
It has à companion about 5 arcsec distant. which corresponds to about LOO AU. | It has a companion about 5 arcsec distant, which corresponds to about 100 AU. |
From infrared photometry this is most likely an M2 chwarf star. | From infrared photometry this is most likely an M2 dwarf star. |
9 Aur A and D are too far apart to interact in any significant way. and the fainter star. being 7 magnitudes fainter in. V. is much too [aint to allect the optical photometry.) | 9 Aur A and B are too far apart to interact in any significant way, and the fainter star, being 7 magnitudes fainter in V, is much too faint to affect the optical photometry.) |
In our search for an explanation. lor 9% Aurigac’s variability one of us (REC) obtained 22 racial velocities with the Coravel racial velocity spectrometer at Haute Provence Observatory. | In our search for an explanation for 9 Aurigae's variability one of us (RFG) obtained 22 radial velocities with the Coravel radial velocity spectrometer at Haute Provence Observatory. |
These were obtained. on 1992. April 23 and from 1993 February 10 to March 24 on a total of 14 nights and showed a range of about 7 km s | These were obtained on 1992 April 23 and from 1993 February 10 to March 24 on a total of 14 nights and showed a range of about 7 km $^{-1}$. |
With an internal error per measurement of about 0.6 kms 1. the variations seemed significant. | With an internal error per measurement of about 0.6 km $^{-1}$, the variations seemed significant. |
Furthermore. a period. of just. under 3 days was indicated. | Furthermore, a period of just under 3 days was indicated. |
What was clearly needed: was a more homogeneous data set one measurement. per hour for as many hours and nights as possible. | What was clearly needed was a more homogeneous data set – one measurement per hour for as many hours and nights as possible. |
Given the type of data Coravel produces. this would also allow us to see if the radial velocities. line widths. fractional line depths. and line profiles vary in à smooth wav from hour to hour and from night to night. | Given the type of data Coravel produces, this would also allow us to see if the radial velocities, line widths, fractional line depths, and line profiles vary in a smooth way from hour to hour and from night to night. |
In this paper we report extensive data runs of photometry and radial velocities of 9 Aur. | In this paper we report extensive data runs of photometry and radial velocities of 9 Aur. |
Given the absence of certain tvpes of evidence (from Paper 1) and the data presented in this paper. we believe we have very strong evidence that 9 Aur is exhibiting non-racial pulsations. | Given the absence of certain types of evidence (from Paper I) and the data presented in this paper, we believe we have very strong evidence that 9 Aur is exhibiting non-radial pulsations. |
Given the time scales involved. they would have to be gravity mocles. | Given the time scales involved, they would have to be gravity modes. |
ln Table 1 we give a summary of the V-band and. B-banel photometry. | In Table 1 we give a summary of the V-band and B-band photometry. |
Phe individual data values can be obtained by requesting LAU file 28512 of Unpublished Observations of Variable Stars. | The individual data values can be obtained by requesting IAU file 285E of Unpublished Observations of Variable Stars. |
Guinans data. reciuced. by AleCook (hereafter. called the Guinan anc AleCook data). were obtained at Alt. Lopkins. Arizona. with two 76-cm Automatic Photoclectric ‘Telescopes (APTS). | Guinan's data, reduced by McCook (hereafter called the Guinan and McCook data), were obtained at Mt. Hopkins, Arizona, with two 76-cm Automatic Photoelectric Telescopes (APTs). |
One APT. is operated by the Four College. Consortium. (PCC). the other by Fairborn Observatory. | One APT is operated by the Four College Consortium (FCC), the other by Fairborn Observatory. |
These two telescopes have photomoeters with matching photomultiplier tubes anc filters. | These two telescopes have photometers with matching photomultiplier tubes and filters. |
Phe APT observations were mace using a 2.5 magnitude neutral density filter to reduce the stars’ count rates to reasonable levels. | The APT observations were made using a 2.5 magnitude neutral density filter to reduce the stars' count rates to reasonable levels. |
Luedeke's data were obtained in Albuquerque. New Alexico. | Luedeke's data were obtained in Albuquerque, New Mexico. |
Wrisciunas’ data were obtained at the 2s800-m elevation. of Alauna Wea. Hawaii. | Krisciunas' data were obtained at the 2800-m elevation of Mauna Kea, Hawaii. |
As in Paper LE the photometry of 9 Aur was obtained by means of differential measures with respect to BS 1561 (= LID 31134: V = |5.78: Sp = A2 V). | As in Paper I, the photometry of 9 Aur was obtained by means of differential measures with respect to BS 1561 (= HD 31134; V = +5.78; Sp = A2 V). |
Ixrisciunas used BS 1568 as a check star. while Luedeke primarily used BS 1668 as a check star. | Krisciunas used BS 1568 as a check star, while Luedeke primarily used BS 1668 as a check star. |
From over 300 dilferential measures with respect to BS 1568 and 38 1668 obtained over several vears. we find no evidence that our principal comparison star. BS 1561. is variable in any wav. | From over 300 differential measures with respect to BS 1568 and BS 1668 obtained over several years, we find no evidence that our principal comparison star, BS 1561, is variable in any way. |
Hence any variations of 9 Aur vs. BS 1561. we attribute solely to 9 Aur. | Hence any variations of 9 Aur vs. BS 1561 we attribute solely to 9 Aur. |
These comparison star vs. check star observations also tell us how accurate an individual dillerential measurement is. | These comparison star vs. check star observations also tell us how accurate an individual differential measurement is. |
For the Guinan ancl MeCook data it is E10 millimagnitudes (mmag) or better. | For the Guinan and McCook data it is $\pm 10$ millimagnitudes (mmag) or better. |
For the Luedeke data the corresponding value is £12 mmag. and for the most recent Ixrisciunas data it is £20 mamas. | For the Luedeke data the corresponding value is $\pm 12$ mmag, and for the most recent Krisciunas data it is $\pm 20$ mmag. |
Guinan's 1903/4 data are averages of 6 to 10 cdilferential measures per point. implving internal errors of 3 t0 5 mmag per point. | Guinan's 1993/4 data are averages of 6 to 10 differential measures per point, implying internal errors of 3 to 5 mmag per point. |
The radial velocities were obtained by REG with the llaute Provence Coravel (Baranne. Mavor Poncet 1979). | The radial velocities were obtained by RFG with the Haute Provence Coravel (Baranne, Mayor Poncet 1979). |
A scanning range of 70 kms |. centred on zero heliocentric velocity. was normally usec and was wide enough to encompass most. (usually all) of the width of the cross-correlation dip. | A scanning range of 70 km $^{-1}$, centred on zero heliocentric velocity, was normally used and was wide enough to encompass most (usually all) of the width of the cross-correlation dip. |
Phe normal integration time was 5 minutes. which in most cases was long enough to give an ample signal but was needed in order to reduce seeing noise’. | The normal integration time was 5 minutes, which in most cases was long enough to give an ample signal but was needed in order to reduce 'seeing noise'. |
Such noise. arising from the fluctuations in the amount of light passing the entrance slit of the Coravel spectrometer. can be objectionable in short integrations. which average too few of the 5-1Iz scans: the elfects are particularly noticeable in traces. such as are given by 9 Aur. exhibiting wide and shallow clips. | Such noise, arising from the fluctuations in the amount of light passing the entrance slit of the Coravel spectrometer, can be objectionable in short integrations, which average too few of the 5-Hz scans; the effects are particularly noticeable in traces, such as are given by 9 Aur, exhibiting wide and shallow dips. |
During one particular observing run (a long run near to opposition of 9 Aur) an intensive series of measurements was made. at rather strictly timed hourly intervals whenever weather and other circumstances permitted. | During one particular observing run (a long run near to opposition of 9 Aur) an intensive series of measurements was made, at rather strictly timed hourly intervals whenever weather and other circumstances permitted. |
On one night as many as 14 consecutive hourly observations were obtained. | On one night as many as 14 consecutive hourly observations were obtained. |
Since Guinan and. AleCook’s latest data represent a number of dillerential measures per point. some averaging was necessary for the Ixrisciunas and. Luedeke data. so that the data would have more comparable weighting. | Since Guinan and McCook's latest data represent a number of differential measures per point, some averaging was necessary for the Krisciunas and Luedeke data, so that the data would have more comparable weighting. |
Given that the minimum number of dilferential measures per night was 3. we averaged the Ixrisciunas ancl Luedeke data by groups of ee | Given that the minimum number of differential measures per night was 3, we averaged the Krisciunas and Luedeke data by groups of 3. |
Given that the minimum number of dilferential measures per night was 3. we averaged the Ixrisciunas ancl Luedeke data by groups of eeJ | Given that the minimum number of differential measures per night was 3, we averaged the Krisciunas and Luedeke data by groups of 3. |
2003). | 2003). |
Also. sources with X-rav spectra consistent with no absorption above the Galactic are plotted: at the Galactic column density.Ng—2107"em.7. | Also, sources with X-ray spectra consistent with no absorption above the Galactic are plotted at the Galactic column density,$\rm N_H=2\times10^{20}\,cm^{-2}$. |
Figure 5.- suggests that the [fraction of X-ray/racio matches increases with the LR or the Ng. | Figure \ref{fig_hr_nh_dist} suggests that the fraction of X-ray/radio matches increases with the HR or the $\rm N_H$. |
About IS vcr cent (4/22) of the population with LR.<O.4 is associated with radio emission while 50im per cent (10/20) of he LR0.4 sources have radio counterparts. | About 18 per cent (4/22) of the population with $\rm HR<-0.4$ is associated with radio emission while 50 per cent (10/20) of the $\rm HR>-0.4$ sources have radio counterparts. |
Similarly. he fraction of N-rav/radio matches is about 23 per cen (6/26) of the population with rest-frame column. density Ἡ«Ίθτο and increases ο about 50 per cen (8/16) for NyLocm. | Similarly, the fraction of X-ray/radio matches is about 23 per cent (6/26) of the population with rest-frame column density $\rm N_H < 10^{22}\, cm^{-2}$ and increases to about 50 per cent (8/16) for $\rm N_H > 10^{22}\, cm^{-2}$. |
However. the small. sample size may bias our conclusions. | However, the small sample size may bias our conclusions. |
We therefore compare the LR and Ng distributions of X-ray selected Ας with ane without radio counterparts using the Gehan’s statistica test as implemented in the package (Isobe. Feigelson Nelson 1986: LaVallev. lsobe Feigelson. 1992). | We therefore compare the HR and $\rm N_H$ distributions of X-ray selected AGNs with and without radio counterparts using the Gehan's statistical test as implemented in the package (Isobe, Feigelson Nelson 1986; LaValley, Isobe Feigelson 1992). |
The probability the two distributions are drawn from the same parent population is rejected at the =95 per cent confidence level correspondingὃν to about 29. | The probability the two distributions are drawn from the same parent population is rejected at the $\approx95$ per cent confidence level corresponding to about $2\sigma$. |
In this section. we focus on the X-rav spectra of. both individual sources and dillerent. groups of X-ray selected ACGNs. | In this section we focus on the X-ray spectra of both individual sources and different groups of X-ray selected AGNs. |
Firstly. we compare the X-ray spectral properties of the ACGNs with and without radio counterparts. comprising 14 and 28 systems respectively The individual spectra of sources in these sub-samples are merged using theMATHPILA task of to produce 3 independent coacdcded spectral files for the PN. MOSI ancl MOS2 detectors respectively. | Firstly, we compare the X-ray spectral properties of the AGNs with and without radio counterparts, comprising 14 and 28 systems respectively The individual spectra of sources in these sub-samples are merged using the task of to produce 3 independent coadded spectral files for the PN, MOS1 and MOS2 detectors respectively. |
The combined spectra are grouped. to a minimum. of 15 counts per bin to ensure that Caussian statistics apply. | The combined spectra are grouped to a minimum of 15 counts per bin to ensure that Gaussian statistics apply. |
Vhe auxiliary files of individual sources were combine using the task ofFrrooLs. | The auxiliary files of individual sources were combined using the task of. |
Using the v11.2 software. we fit a single power-law to the data. absorbec bv the Galactic column of 2107em7? (wabs*pow). | Using the v11.2 software, we fit a single power-law to the data absorbed by the Galactic column of $\rm
2\times 10^{20}\,cm^{-2}$ (wabs*pow). |
The results are presented. in “Table 3. | The results are presented in Table \ref{tbl_res1}. |
N-rav/radio matchec AGNs have Blatter spectra. (Lo=LTS ($052) than non-radio detected. sources (P.=2.00 val) at the =da significance level. | X-ray/radio matched AGNs have flatter spectra $\Gamma=1.78^{+0.05}_{-0.03}$ ) than non-radio detected sources $\Gamma=2.00^{+0.03}_{-0.04}$ ) at the $\approx4\sigma$ significance level. |
A similar result was obtained by Bauer e al. ( | A similar result was obtained by Bauer et al. ( |
2002). who explored the association between the fain X-ray kkeV) and racio 6GCGLIz) source populations detected in the IIubble Deep Field North region using the LAIMIsChandra dataset ancl ultra-cdeep VLA observations. | 2002), who explored the association between the faint X-ray keV) and radio GHz) source populations detected in the Hubble Deep Field North region using the Ms dataset and ultra-deep VLA observations. |
Although their sample is dominated: by. starbursts. they also identify a number of X-ray selected Αλ ancl argue that those with radio cleteetions have harder X-ray. spectral properties than radio undetected ones. | Although their sample is dominated by starbursts, they also identify a number of X-ray selected AGNs and argue that those with radio detections have harder X-ray spectral properties than radio undetected ones. |
Dauer et al. ( | Bauer et al. ( |
2002) sugeest that the enhanced: absorption observed. in. racio detected ACGNSs is due to nuclear starbursts. | 2002) suggest that the enhanced absorption observed in radio detected AGNs is due to nuclear starbursts. |
We explore this scenario using X-rav spectral fitting analysis of the hard (vest-Lrame Ny107em ?) X-pavfracio matched: sources in the survey. | We explore this scenario using X-ray spectral fitting analysis of the hard (rest-frame $\rm N_H>10^{22}\,cm^{-2}$ ) X-ray/radio matched sources in the survey. |
Although individual sources have a small number of counts. which do not allow detailed spectral analysis. we can | Although individual sources have a small number of counts, which do not allow detailed spectral analysis, we can |
and (see Snyder et al. | and (see Snyder et al. |
1997) where s is a subseript indicating particle species (p for proton and e for electron). f, is the distribution function of particle species s. my and e, are the mass and charge ofu speciesο s. Ὁ is. particleο velocity.. η=b:Tv. vp—c(E«B)/B.? uu—JavbTvi]yd(2B, Uy)—Ub. and D/Dt=9/9:|eg):V. | 1997) where $s$ is a subscript indicating particle species (p for proton and e for electron), $f_s$ is the distribution function of particle species $s$, $m_s$ and $e_s$ are the mass and charge of species $s$ , $\bm{v}$ is particle velocity, $v_\parallel = \bm{\hat{b}} \cdot
\bm{v}$ , $\bm{v}_{E} = c (\bm{E}\times\bm{B})/B^2$, $\mu = |\bm{v} -
v_\parallel \bm{\hat{b}} - \bm{v}_{E}|^2/2B$, $U_\parallel = \bm{U}
\cdot \bm{\hat{b}}$, and $D/Dt = \partial /\partial t + (v_\parallel
\bm{\hat{b}} + \bm{v}_{E}) \cdot \bm{\nabla}$. |
In Equation (A9). f, is regarded as a function of position a. time 7. magnetic moment µ. and parallel velocity v|. | In Equation \ref{eq:dfdt}) ), $f_s$ is regarded as a function of position $\bm{x}$, time $t$, magnetic moment $\mu$, and parallel velocity $v_\parallel$. |
(6Rather than retain the subscripts on the number densities. we define which is also equal to ης because of Equation (A7)). | Rather than retain the subscripts on the number densities, we define which is also equal to $n_{\rm e}$ because of Equation \ref{eq:quasineutrality}) ). |
We have neglected the electron contribution to the mass density. setting p The parallel and perpendicular temperatures are related to the parallel and perpendicular pressures defined above in the usual mu.way: pj,—ΠΚΕΤις and pj,=n&pT|.. | We have neglected the electron contribution to the mass density, setting $\rho = n m_{\rm p}$ The parallel and perpendicular temperatures are related to the parallel and perpendicular pressures defined above in the usual way: $p_{\perp \rm s} = n k_{\rm B} T_{\perp \rm s}$ and $p_{\parallel \rm s} = n k_{\rm B} T_{\parallel \rm s}$. |
? extended Kulsrud's collisionless MHD to account for collisions by adding a BGK collision operator (?) to the right-hand side of Equation (A9)). | \cite{snyder97} extended Kulsrud's collisionless MHD to account for collisions by adding a BGK collision operator \citep{gross56} to the right-hand side of Equation \ref{eq:dfdt}) ). |
For the case we consider here. in which the electrons and ions have the same average velocity U and number density η. this collision operator takes the form where is a shifted Maxwellian with temperature and v4 is the collision frequency for momentum exchange between species » and species k. ( | For the case we consider here, in which the electrons and ions have the same average velocity $\bm{U}$ and number density $n$, this collision operator takes the form where is a shifted Maxwellian with temperature and $\nu_{sk}$ is the collision frequency for momentum exchange between species $s$ and species $k$. ( |
Here. we neglect energy exchange between protons and electrons. but we include it in section 2..) | Here, we neglect energy exchange between protons and electrons, but we include it in section \ref{sec:fluxtube}. .) |
?. then obtained a hierarchy of fluid equations by multiplying Equation (A9)) by various powers of v, and µ and then integrating over v| and µ. | \cite{snyder97} then obtained a hierarchy of fluid equations by multiplying Equation \ref{eq:dfdt}) ) by various powers of $v_\parallel$ and $\mu$ and then integrating over $v_\parallel$ and $\mu$ . |
For the protons, the equations for στρ and pj, can be written (2?) anc where mp 1s the proton mass. and In Section 2 we neglect the term in Equation (A18)) because it is smaller than the proton-proton Coulomb collision frequency. | For the protons, the equations for $p_{\perp
\rm p}$ and $p_{\parallel \rm p}$ can be written \citep{snyder97,sharma06a}
and where $m_{\rm p}$ is the proton mass, and In Section \ref{sec:fluxtube} we neglect the $\nu_{\rm pe}$ term in Equation \ref{eq:nup})) because it is smaller than the proton-proton Coulomb collision frequency. |
Our qj, is by definition a factorvy, of 2 smaller than Snyder et al. | Our $q_{\parallel \rm p}$ is by definition a factor of 2 smaller than Snyder et al. |
’s(1997).In this appendix. the Lagrangian time derivative is given by | 's(1997).In this appendix, the Lagrangian time derivative is given by |
of primordial D/II aud the hydrogen Lxiuau series. lines can be followed down to Lv12. | of primordial D/H and the hydrogen Lyman series lines can be followed down to Ly12. |
We used a \? minimization routine (Fontana Dallester 1995) iu to fit Voiet profiles to the observed. absorption profiles. and obtain for cach fitted absorption componcut the wavelength. the column density XN. the Doppler parameter b aud the corresponding errors. | We used a $\chi^2$ minimization routine (Fontana Ballester 1995) in to fit Voigt profiles to the observed absorption profiles, and obtain for each fitted absorption component the wavelength, the column density $N$, the Doppler parameter $b$ and the corresponding errors. |
Iu the case of igh hydrogen column deusities like iu DLA systems. we expect the neutral and low iouization netal lines to trace. the IL. therefore we model the Lui seies to Lyl2) absorption profiles with three catures corresponding to the two main components (2 and 3) and the reddest component (7) as determined from he metal lines (Fig. 1)). | In the case of high hydrogen column densities like in DLA systems, we expect the neutral and low ionization metal lines to trace the H, therefore we model the Lyman series $\beta$ to Ly12) absorption profiles with three features corresponding to the two main components (2 and 3) and the reddest component (7) as determined from the metal lines (Fig. \ref{low-ion}) ). |
The contribution of the weaker conrponeut 7 is required only to better constrain the fit ou he red edge of the Lyman lines. | The contribution of the weaker component 7 is required only to better constrain the fit on the red edge of the Lyman lines. |
The relative iuteusities of hese three major hyvdroseenOo components were scaled with he metal lines assunune they have approxinativelv the sale abundance ratios from componcut to coupoucut. | The relative intensities of these three major hydrogen components were scaled with the metal lines assuming they have approximatively the same abundance ratios from component to component. |
Starting from this basis we obtained the final column deusities aud b-values (free parameters) by fitting simultaneously the lines of the Lyman series and by assunine the same redshift for the three IT components as for the metal lines. | Starting from this basis we obtained the final column densities and $b$ -values (free parameters) by fitting simultaneously the lines of the Lyman series and by assuming the same redshift for the three H components as for the metal lines. |
The Lay} absorption profile provides a very eood coustraiut to the total column density and the Lys. Lx9. LylO and Lyl2 profiles (which are the ones free from stroug contamination) to the b-walues. | The $\beta$ absorption profile provides a very good constraint to the total column density and the Ly8, Ly9, Ly10 and Ly12 profiles (which are the ones free from strong contamination) to the $b$ -values. |
From the best fit (Fig. 2.. | From the best fit (Fig. \ref{Lyb}, |
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