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. As a consequence. ratios may be underestimated by a factor of 2 if derived from the main isotopologue. | As a consequence, ratios may be underestimated by a factor of $\sim 2$ if derived from the main isotopologue. |
The — column density. presents a significant uncertainty due to its blending with the newly detected isotopologue of methanol. SCILOIL | The $^+$ column density presents a significant uncertainty due to its blending with the newly detected isotopologue of methanol, $^{13}$ $_3$ OH. |
However. the abundance should not be affected by more than a factor of 2. | However, the $^+$ abundance should not be affected by more than a factor of 2. |
We have derived a column density for MCLL,OLL of ~1.6010)xI0!em 7. | We have derived a column density for $^{13}$ $_3$ OH of $\sim1.6(1.0)\times10^{14}\,\rm cm^{-2}$ . |
Lf we compare this columndensity. with that of the main isotopologue from it results ina ΟΙ ΟΠΗ ΟΙ ratio of 1247. significantly lower than the ratio I20/P 0-40 (Henkeletal.1993). | If we compare this columndensity with that of the main isotopologue from \citep{Martin06b} it results in a $_3$ $^{13}$ $_3$ OH ratio of $12\pm7$, significantly lower than the ratio $^{12}$ $^{13}$ C=40 \citep{Henkel93}. |
. Both the difference of 6" in the observed. positions and a different [filling factor of ΟΙ might account for part of this dillerence. | Both the difference of $6''$ in the observed positions and a different filling factor of $_3$ OH might account for part of this difference. |
However. the integrated intensities measured [for (he methanol eroup of transitions at GGllIz by Martinetal.(200Gb) and IHiüttemeisterοἱal.(1997) at positions differing by >13” show a variation of <6% so the dilference in positions is not likely to contribute to this difference. | However, the integrated intensities measured for the methanol group of transitions at GHz by \citet{Martin06b} and \citet{Hutte97}
at positions differing by $>13''$ show a variation of $<6\%$ so the difference in positions is not likely to contribute to this difference. |
Thus. opacity is likely (he dominant effect as observed in (he Galactic center 2006).. | Thus, opacity is likely the dominant effect as observed in the Galactic center \citep[GC,][]{Requena06}. . |
From the |C/UC ratioin 2253 we derive a fractional abundance of methanol of 10. *. close to the abundances observed in the Galactic center (Requena-Torresetal. 2006).. | From the $^{12}$ $^{13}$ C ratioin 253 we derive a fractional abundance of methanol of $\sim$ $^{-7}$, close to the abundances observed in the Galactic center \citep{Requena06}. . |
Methanol is. after CO and NO. the most abundant molecule | Methanol is, after CO and NO, the most abundant molecule |
uubiascd estimates of the Sérrsic iudex ancl effective radius for galaxies with S/N»LO aud r.>0.03". independenutlv of the redshift of the source. thus demonstrating that the surface brightuess cine is nof an dssue for this kind of studies. | unbiased estimates of the Sérrsic index and effective radius for galaxies with $>10$ and $r_e>0.03'',$ independently of the redshift of the source, thus demonstrating that the surface brightness dimming is not an issue for this kind of studies. |
The PSF was obtained i each passband ποσα bv averaging welbexposed. uusaturated stars; | The PSF was obtained in each passband needed by averaging well-exposed, unsaturated stars. |
We runi GALFIT experimenting on various sizes of the fittiug reeion around each galaxy. aud with the sky either set to a preaueasured value or left as à free parameter. | We run GALFIT experimenting on various sizes of the fitting region around each galaxy, and with the sky either set to a pre-measured value or left as a free parameter. |
We verified that the sizes aud Sévrsic iudices do not vary by iore than in the various cases. | We verified that the sizes and Sérrsic indices do not vary by more than in the various cases. |
The values that we show throughout the paper were obtained with a free sky and 6<6 arcsec? fittine regions. | The values that we show throughout the paper were obtained with a free sky and $6\times6$ $^2$ fitting regions. |
Auy closeby object detected by SExtractor within cach fitting region was automatically masked out during the fitting procedure. | Any closeby object detected by SExtractor within each fitting region was automatically masked out during the fitting procedure. |
Finally. we selected a sample of local galaxies frou the Sloan Dieital Sky Survey (SDSS). for which masses. star formation rates and morphological parameters are available in literature. | Finally, we selected a sample of local galaxies from the Sloan Digital Sky Survey (SDSS), for which masses, star formation rates and morphological parameters are available in literature. |
In particubku. we combined the MPA SDSS DR7 catalog. that contains stellis masscs and star formation rates (lxauffüiiaun et al. | In particular, we combined the MPA SDSS DR7 catalog, that contains stellar masses and star formation rates (Kauffmann et al. |
2003: Brinchinann et al. | 2003; Brinchmann et al. |
2001) with the DR? NYU Valuc-Added Galaxy Catalog. that coutains the CALFIT Séirsic best fit to the m g. r. / aud 2 SDSS images (Blanton et al. | 2004) with the DR7 NYU Value-Added Galaxy Catalog, that contains the GALFIT Sérrsic best fit to the $u$, $g$, $r$, $i$ and $z$ SDSS images (Blanton et al. |
2005). | 2005). |
We defined the local sample of massive and passive early-type galaxies by applying the sale criteria used for the ligh-: oues: stellar 1iass AL.>1010 aud specific star formation rate SSFR<LO2Gyr.|. | We defined the local sample of massive and passive early-type galaxies by applying the same criteria used for the $z$ ones: stellar mass $M_{\odot}>10^{10}$ and specific star formation rate $<10^{-2} Gyr^{-1}$. |
Tusteacd of visually inspecting the whole sample. we eliminated the disk dominated objects removing all the objects of the total) with Sérrse index s<2 im the r baud. | Instead of visually inspecting the whole sample, we eliminated the disk dominated objects removing all the objects of the total) with Sérrsic index $s<2$ in the $r-$ band. |
We verified with a random sample of 200 SDSS ealaxics that the contamination of disk dominated objects among objects with s>2 is below | We verified with a random sample of 200 SDSS galaxies that the contamination of disk dominated objects among objects with $s>2$ is below. |
Iu Figure 5. we compare the Sérrsic indices aud the physical sizes in the UV and optical rest-frames. for the high aud low redshift suuples. | In Figure \ref{fig3} we compare the Sérrsic indices and the physical sizes in the UV and optical rest-frames, for the high and low redshift samples. |
Since the errors ou the sizes and Sérrsic indices given by GALEIT are the formal errors derived by the fitting procedure aud do not take iuto account anv systematic wacertaity. m this Figure and in the following we set the error bars to a nuünimuuin value of | Since the errors on the sizes and Sérrsic indices given by GALFIT are the formal errors derived by the fitting procedure and do not take into account any systematic uncertainty, in this Figure and in the following we set the error bars to a minimum value of . |
For the low redshift sample we restricted the analysis at z>0.6. and we used the ACS e band and + band. matching the rest-frame UV and optical. respectively. | For the low redshift sample we restricted the analysis at $z>0.6$, and we used the ACS $v-$ band and $z-$ band, matching the rest-frame UV and optical, respectively. |
We did not iuclude galaxies at lower redshift. as the UV rest-frame at i<0.6 would be matched by the ACS/B-hand. that provides a worse S/N than the other ACS bands. | We did not include galaxies at lower redshift, as the UV rest-frame at $z<0.6$ would be matched by the ACS/B-band, that provides a worse S/N than the other ACS bands. |
As we already. said iu the previous section. the τ~2 sample coutains the 52 ealaxiesfor which the WECS3 imaging is available: at that redshift. the + and the £7-haucl correspond respectively to the rest-frame UV at ~3000A aud optical at ~5STOOA. | As we already said in the previous section, the $z\sim2$ sample contains the 52 galaxiesfor which the WFC3 imaging is available: at that redshift, the $z-$ and the $H$ -band correspond respectively to the rest-frame UV at $\sim$ and optical at $\sim$. |
. First of all. of the passive ealaxies at τσL2 aud Do2 have a Sérrsic index s=2. both at UV aud optical wavelengths. | First of all, of the passive galaxies at $z<1.2$ and $z\sim2$ have a Sérrsic index $s>2$, both at UV and optical wavelengths. |
This is not surprising. as the sample has been restricted to contain only visually classified spheroidals. | This is not surprising, as the sample has been restricted to contain only visually classified spheroidals. |
Secoudly. the sizes iicasured in the UV and in the optical correlate almost perfectly with cach otler. with a scatter snaller than 420%.. | Secondly, the sizes measured in the UV and in the optical correlate almost perfectly with each other, with a scatter smaller than $\pm$. |
. The Sérrsic indices iui he two rest-frame bands are correlate as well. but show a lareer scatter (~10543). | The Sérrsic indices in the two rest-frame bands are correlate as well, but show a larger scatter $\sim40$ ). |
Tlowever. we do see systematic offsets for both sizes and Sérrsic indices in the two rest-renes. that become more evident when checking the ractional differences between optical and UV. shown iu he insets of Figure 3.. | However, we do see systematic offsets for both sizes and Sérrsic indices in the two rest-frames, that become more evident when checking the fractional differences between optical and UV, shown in the insets of Figure \ref{fig3}. |
We see that on average galaxies at L2«—i«2.5 have sizes smaller iid Sérrsic indices larger in the optical than in the UV rest-rane. | We see that on average galaxies at $1.2<z<2.5$ have sizes smaller and Sérrsic indices larger in the optical than in the UV rest-frame. |
Sumuilaurlv. galaxies at 0.6<+«1.2 galaxies lave sizes smaller sand Sérrsbe indices Lhueer in the optical than in the UW rest-frame. | Similarly, galaxies at $0.6<z<1.2$ galaxies have sizes smaller and Sérrsic indices larger in the optical than in the UV rest-frame. |
This reinforces our previous result prescuted in Cassata ct al. ( | This reinforces our previous result presented in Cassata et al. ( |
2010). where we showed a sinular trend for the subset of galaxies at 2~ Wing in the IIUDE. and it is du οσους aercement with other studies of carly-type galaxies at 2~ (AleCarthy et al. | 2010), where we showed a similar trend for the subset of galaxies at $z\sim2$ lying in the HUDF, and it is in good agreement with other studies of early-type galaxies at $z\sim2$ (McCarthy et al. |
2007: Trujillo et al. | 2007; Trujillo et al. |
2007: Ryan et al. | 2007; Ryan et al. |
2011). as well as at lower redshift (Papovich et al. | 2011), as well as at lower redshift (Papovich et al. |
2003: Cassata et al. | 2003; Cassata et al. |
2005). | 2005). |
Iuterestiuglv. these biases basically iniplv. that carl-type galaxies at +>>1.2 show a uceative color gradient. with the center beime redder than the outskirts. | Interestingly, these biases basically imply that early-type galaxies at $z>1.2$ show a negative color gradient, with the center being redder than the outskirts. |
Earltypes at lower redshift show a simular. butshallower. color eracicnt. | Early-types at lower redshift show a similar, butshallower, color gradient. |
This is iu very good agreement with the results by Coro et al. ( | This is in very good agreement with the results by Guo et al. ( |
20115). who found negative color eracdieuts for 6 passive galaxies in IIUDE. steeper than those observed iu local early-type galaxies. | 2011b), who found negative color gradients for 6 passive galaxies in HUDF, steeper than those observed in local early-type galaxies. |
Based on these evidences. we can conclude that iu the whole 0.<:«2.5 interval the morphological Is-correction is weak for passive spheroidals that have already euded their star formation activity. | Based on these evidences, we can conclude that in the whole $0<z<2.5$ interval the morphological K-correction is weak for passive spheroidals that have already ended their star formation activity. |
Tn Figure Lo we show the mass-size relation for the 52 ealanics at 1.2τς2.5 selected in the ERS|IITUDE WECS3 fields. in the same three redshift bins of Figure 2.. | In Figure \ref{fig4} we show the mass-size relation for the 52 galaxies at $1.2<z<2.5$ selected in the ERS+HUDF WFC3 fields, in the same three redshift bins of Figure \ref{fig2}. |
The sizes have been measured by CALFIT in the Fl60w filter. that at these redshifts corresponds to the optical rest-frame regine. | The sizes have been measured by GALFIT in the F160w filter, that at these redshifts corresponds to the optical rest-frame regime. |
We plot as well the mass-size relation for local ETGs drawn from the SDSS. in the sale optical rest-frame. | We plot as well the mass-size relation for local ETGs drawn from the SDSS, in the same optical rest-frame. |
We stress that here the mass mcasurements were homogenized to a Salpeter IME (see Section 2 for details). | We stress that here the mass measurements were homogenized to a Salpeter IMF (see Section 2 for details). |
The relation for SDSS passive ealaxies is found to be iu good agreciment with results by Shen et al. ( | The relation for SDSS passive galaxies is found to be in good agreement with results by Shen et al. ( |
2003). that are widely used by may autlors as a reference at 2—0. | 2003), that are widely used by many authors as a reference at $z\sim0$. |
At all redshifts. we callcompact any carly-type galaxies 0.1 dex smaller than local SDSS galaxies of the same mass. aud.compact auv ealaxv Loo below the local relation. | At all redshifts, we call any early-type galaxies 0.4 dex smaller than local SDSS galaxies of the same mass, and any galaxy $1-\sigma$ below the local relation. |
The first definition cones out naturally as the maxinuun size without a counterpart in the local universe (see Section 5): the second is the least strict definition of used in the literature and in this wav we can compare our mcasurements with others. | The first definition comes out naturally as the maximum size without a counterpart in the local universe (see Section 5); the second is the least strict definition of used in the literature and in this way we can compare our measurements with others. |
Thenormal ETGs are those liug outop or above the local relation. | The ETGs are those lying ontop or above the local relation. |
If we define the ican Inass deusitv within the half liebt radius as: we note that the local relation is roughly parallel tothe locii of constant Msy. | If we define the mean mass density within the half light radius as: we note that the local relation is roughly parallel tothe locii of constant $\Sigma_{50}$ . |
Compact and ultra-compact ETCs have mass densities XzyZ3«10AFApe7? and Mau2L.21019AFepe: 7. respectively. | Compact and ultra-compact ETGs have mass densities $\Sigma_{50}\gtrsim3\times10^{9}M_{\odot} kpc^{-2}$ and $\Sigma_{50}\gtrsim1.2\times10^{10}M_{\odot} kpc^{-2}$ , respectively. |
For cach redshift bin we show the region of the plane where our selection detects at least of the objects. | For each redshift bin we show the region of the plane where our selection detects at least of the objects. |
To | To |
more significant contribution by background dust than their corresponding mirror cells in the north. | more significant contribution by background dust than their corresponding mirror cells in the north. |
In the region |b]«0.5". the north-south asymmetry is substantially reciuced and. interestingly enough. most cases now have clicsouthfioserio82 1.0. | In the region $|b|<0.5^{\circ}$, the north-south asymmetry is substantially reduced and, interestingly enough, most cases now have $A_{K,south}/A_{K,north} \approx$ 1.0. |
TFhis applies to both FIR and 2ALASS data. the main dillerence. between the wo datasets being the larecr dispersion in the south/north values in the former relative to the later. | This applies to both FIR and 2MASS data, the main difference between the two datasets being the larger dispersion in the south/north values in the former relative to the later. |
Interpreting this north-south asymmetry is not an easy ask. | Interpreting this north-south asymmetry is not an easy task. |
The similarity of the histograms in panel (lta) plus our model predictions suggest that extinction in the 3<b|«5° strips is dominated: by foreground. structure. in he form of extended. dust. clouds. (see also map in Fig. | The similarity of the histograms in panel (14a) plus our model predictions suggest that extinction in the $3^{\circ}<{\it |b|}<5^{\circ}$ strips is dominated by foreground structure in the form of extended dust clouds (see also map in Fig. |
3 and the concluding section). | 3 and the concluding section). |
At lower latitudes. the extinction values increase and become dominated by dilluse dust. clistribution or by dense clouds located close to the Galactic centre. | At lower latitudes, the extinction values increase and become dominated by diffuse dust distribution or by dense clouds located close to the Galactic centre. |
In these cases. the shape and position of 16 AKsehfAery histograms in both datasets should reflect the global properties of the dust. distribution rather iui the contribution. of any individual cust cloud. | In these cases, the shape and position of the $A_{K,south}/A_{K,north}$ histograms in both datasets should reflect the global properties of the dust distribution rather than the contribution of any individual dust cloud. |
As rw FIR data reach deeper into the dust. columns than 10 PALASS. the transition from the foreground. dominated regime to one dominated by the global distribution starts arlier in the former dataset: this ellect is the likely cause of 1e dillerence in the histograms in panel (14b). | As the FIR data reach deeper into the dust columns than the 2MASS, the transition from the foreground dominated regime to one dominated by the global distribution starts earlier in the former dataset; this effect is the likely cause of the difference in the histograms in panel (14b). |
In the b<0.5% strip. the νονος values are strongly imited by optical depth and largely unreliable (Sect. | In the $|b|<0.5^{\circ}$ strip, the $A_{K,2MASS}$ values are strongly limited by optical depth and largely unreliable (Sect. |
2.1). while the laceya values are suller from the effects of dust reated bevoncl 21Ix.. Despite these uncertainties the dust distribution in this region is reasonably svnimetric. | 2.1), while the $A_{K,FIR}$ values are suffer from the effects of dust heated beyond 21K. Despite these uncertainties the dust distribution in this region is reasonably symmetric. |
There is a small trend. in the sense o£ lgsoupτννοDol. especially in the EI data. | There is a small trend in the sense of $A_{K,south}/A_{K,north} > 1$, especially in the FIR data. |
This trend. is intriguing. | This trend is intriguing. |
The fact that most cells have [larger μι values at southern latitucles than at northern ones may be telling us something about the ecometry of the dust. distribution relative to the Sun's position. | The fact that most cells have larger $A_{K,FIR}$ values at southern latitudes than at northern ones may be telling us something about the geometry of the dust distribution relative to the Sun's position. |
In order to take into account a possible displacement by the Sun relatively to the disk mid-plane. we again use our nmocel presented in Sect. | In order to take into account a possible displacement by the Sun relatively to the disk mid-plane, we again use our model presented in Sect. |
4.1. | 4.1. |
Considering the Sun displaced bv 5. 15 and 25pe above the Plane. we obtain typical south/north ratios in the 7; or τι values of 1.08. 1.27 and 1.50. respectively. | Considering the Sun displaced by 5, 15 and 25pc above the Plane, we obtain typical south/north ratios in the $\tau_{8.5}$ or $\tau_{\infty}$ values of 1.08, 1.27 and 1.50, respectively. |
However. the model does not incorporate any asymmetry caused. by foreground. dust. clouds. which seems to be the dominant elfect generating the asymmetry in the 2ALASS and FIR data. | However, the model does not incorporate any asymmetry caused by foreground dust clouds, which seems to be the dominant effect generating the asymmetry in the 2MASS and FIR data. |
Lt is thus impossible at the present to quantify the Sun's displacement from the cise based on the data. | It is thus impossible at the present to quantify the Sun's displacement from the disc based on the data. |
We should. point out. that Unavane et al. ( | We should point out that Unavane et al. ( |
1998). using DIENIS data. also concluded that the asvmametry in the inner Dulge extinction is dominated. by foreground dust. clouds. | 1998), using DENIS data, also concluded that the asymmetry in the inner Bulge extinction is dominated by foreground dust clouds. |
We built the extinction map towards the central 10 of the Galaxy. using the 2ALASS Point Source Catalog. | We built the extinction map towards the central $10^{\circ}
\times 10^{\circ}$ of the Galaxy using the 2MASS Point Source Catalog. |
We extracted J and WKY magnitudes for about 6 million stars in the range NS<A.13.0. | We extracted J and $_s$ magnitudes for about 6 million stars in the range $8.0 \le {\it K_s} \le 13.0$. |
The adopted. map resolution is 44. | The adopted map resolution is $^{\prime} \times 4^{\prime}$. |
Lt was possible to obtain extinction values for S80 of the 32.761 cells defined. in the area. where 2ALASS data were currently available and a Bulge eint branch was distinct enough. | It was possible to obtain extinction values for $\approx$ 80 of the 32,761 cells defined in the area, where 2MASS data were currently available and a Bulge giant branch was distinct enough. |
The extinction alfecting he bulk of the Bulge stellar population was determined wo matching the upper elant branch found in theA. A.) colour magnitude diagram to the reference upper giant xanch built using ce-redcdened Bulge fields. | The extinction affecting the bulk of the Bulge stellar population was determined by matching the upper giant branch found in the, ) colour magnitude diagram to the reference upper giant branch built using de-reddened Bulge fields. |
Phe extinction values vary [rom —0.05 in the edges of the map up to ely=2 close to the Galactic centre. | The extinction values vary from =0.05 in the edges of the map up to =3.2 close to the Galactic centre. |
The mean extinction ound is «τν=0.29 with a dispersion o=0.12: 63% of the cells are within2-7 of the mean. | The mean extinction found is ${\it<A_K>}=0.29$ with a dispersion $\sigma = 0.12$; 63 of the cells are within$\sigma$ of the mean. |
We compared. our 2ALASS extinction. map to. that of Schultheis et al. ( | We compared our 2MASS extinction map to that of Schultheis et al. ( |
1999) in the region |/|]«5° and peLs which is common to both studies. | 1999) in the region $|\ell| <5^{\circ}$ and $|{\it b}|<1.5^{\circ}$, which is common to both studies. |
Schultheis et al. | Schultheis et al. |
extinction map is based on DENIS photometry. | extinction map is based on DENIS photometry. |
We find an excellent agreement between the two extinction determinations. especially upto ly=1.0. | We find an excellent agreement between the two extinction determinations, especially up to ${\it A_K}=1.0$. |
Bevone this limit the values derived from the DENIS data are svstematically larger. | Beyond this limit the values derived from the DENIS data are systematically larger. |
This small discrepancy in large extinction regions is not unexpected. considering. the photometric errors. incompleteness effects. and uncertainties in. extinction determination. | This small discrepancy in large extinction regions is not unexpected, considering the photometric errors, incompleteness effects, and uncertainties in extinction determination. |
Me:so compared the present extinction map to that of Schlegel ct al. ( | We also compared the present extinction map to that of Schlegel et al. ( |
1998). which is based on dust. emission in the far infrared detected by the DIRBE/IRAS instruments. | 1998), which is based on dust emission in the far infrared detected by the DIRBE/IRAS instruments. |
As the data from the latter are allected by the entire dust column. with no depth limit. the comparison was mace separately for regions of decreasing Galactic latitude:6. which supposedly correspond. to increasing contribution bv dust located on the background of the Galactic Centre. | As the data from the latter are affected by the entire dust column, with no depth limit, the comparison was made separately for regions of decreasing Galactic latitude, which supposedly correspond to increasing contribution by dust located on the background of the Galactic Centre. |
The background dust contribution was estimated by means of a double exponential dust distribution model. | The background dust contribution was estimated by means of a double exponential dust distribution model. |
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