text:
\section{Introduction}\label{sec:Introduction}

The evolution of an isolated spiral galaxy is regulated by the cooling and accretion of the circum-galactic medium (CGM), the condensation of the cool gas in the disk and the follow-up star formation, as well as the feedback of energy and metal-enriched material by young stars and supernovae (SNe) back into the interstellar medium (ISM) and the CGM. In these processes, molecular gas in the galactic disk acts as a link for gas cycling between the CGM (via cooling and accretion) and the star formation (by providing fuel) (e.g., \citealt{Kennicutt12,Bolatto13} and references therein). Therefore, measuring the overall content and spatial distribution of molecular gas in an isolated spiral galaxy plays a key role in understanding how it builds up the stellar content of the galaxy.

A spiral galaxy is not expected to survive a few major mergers, so the most massive galaxies in the local universe are always giant ellipticals in the center of clusters of galaxies. However, there exist extremely massive spiral galaxies with stellar mass a few times of the Milky Way (MW) in the local universe. These galaxies often have specific star formation rates (${\rm sSFR}={\rm SFR}/M_*$, where SFR and $M_*$ are the star formation rate and stellar mass of the galaxy) comparable to or lower than that of the MW, so it is impossible to build up their huge stellar mass with just continuous star formation at the current rate (e.g., \citealt{Li17}). Galaxy archeology with globular clusters (GCs) reveals that there are at least two stellar populations in massive spirals, associated with the disk and bulge respectively, with the disk component typically younger and with higher metallicity (e.g., \citealt{Cezario13}). This bimodality in the age and metallicity of GCs indicates that the major part of the disk of these galaxies may form after the merger and starburst stage when the galaxy swallowed most of the companions and became dominant in the dark matter halo. This scenario is further supported by the discovery of superluminous ($M_*=0.3-3.4\times10^{11}\rm~M_\odot$) spiral galaxies with active star formation (${\rm SFR}=5-65\rm~M_\odot~yr^{-1}$), diverse environments and merger stages at $z\sim0.1-0.3$ \citep{Ogle16}. These galaxies may be the progenitors of the local massive, isolated, quiescent spiral galaxies which represent the cleanest cases to witness the gentle growth of galactic disks without major merger and extensive star formation.

The above scenario indicates that the massive spiral galaxies observed in the local universe may have the major gas supply cutoff and the star formation stopped (also see discussions in \citealt{Schawinski14}). In this case, the leftover cold gas is quite informative in our understanding of the star formation, gas budget, and feedback efficiency in the post-starburst stage. We need to answer a few key questions to understand the formation of these extremely massive spiral galaxies, such as: (1) What is the amount and spatial distribution of the molecular gas? Do they maintain a regular, enhanced, or reduced star formation in the post starburst stage? (2) Is the gas circulation between the galaxy and CGM sufficient to maintain the observed amount of cold gas and star formation? (3) How does the existence of cold gas affect the feedback efficiency?

The Circum-Galactic Medium of MASsive Spirals (CGM-MASS) is a project studying the multi-phase CGM around the most massive (rotation velocity $v_{\rm rot}>300\rm~km~s^{-1}$, stellar mass $M_*\gtrsim1.5\times10^{11}\rm~M_\odot$) isolated spiral galaxies in the local universe \citep{Li16b,Li17,Li18}. The sample includes five galaxies observed in an \emph{XMM-Newton} AO-13 large program plus a few galaxies with high quality archival X-ray data. All of the sample galaxies appear to be less active in star formation than the star formation main sequence of low redshift galaxies (e.g., \citealt{Chang15}). None of them are in dense environments such as galaxy clusters. In order to study the molecular gas properties of these massive isolated quiescent spiral galaxies, we obtained deep IRAM 30m observations of the molecular lines of seven of the CGM-MASS galaxies visible in the northern sky in the 2016B, 2017A, and 2018B semesters with a total observing time of 25.2~hours.

In this paper, we focus on the initial results from the IRAM 30m observations of NGC~5908, which has the highest quality data and is the nearest galaxy in the CGM-MASS sample (\citealt{Li16b,Li17}; see basic parameters of NGC~5908 in Table~\ref{table:NGC5908}). NGC~5908 is a highly-inclined massive spiral galaxy. We adopt a SFR estimated from the \emph{WISE} $22\rm~\mu m$ data ($3.8\pm0.1\rm~M_\odot~yr^{-1}$; \citealt{Li17}), which is $\approx43\%$ of what is obtained from the low-resolution \emph{IRAS} data \citep{Li16b}, and is consistent with the measured radio flux \citep{Condon02} and the radio-IR relation of edge-on galaxies (e.g., \citealt{Li16a}). The resultant specific SFR and SFR surface density are ${\rm SFR}/M_*=0.15\rm~M_\odot~yr^{-1}/(10^{10}\rm~M_\odot)$ and $\Sigma_{\rm SFR}=3\times10^{-3}\rm~M_\odot~yr^{-1}~kpc^{-2}$ (assuming the radius of the star forming disk is $r=20\rm~kpc$), respectively, both comparable to that of the MW \citep{Robitaille10,McMillan11}. For comparison, typical starburst galaxies have far larger ${\rm SFR}/M_*$ and $\Sigma_{\rm SFR}$ of $\gtrsim1\rm~M_\odot~yr^{-1}/(10^{10}\rm~M_\odot)$ and $\gtrsim10^{-2}\rm~M_\odot~yr^{-1}~kpc^{-2}$ (e.g., \citealt{Li13a,Li13b,Wang16}). Therefore, we regard NGC~5908 as a star formation inactive galaxy.
In the present paper, we will present data reduction in \S\ref{sec:datareduction}, main results and discussions in \S\ref{sec:resultsdiscussion}, and summarize the major conclusions in \S\ref{sec:summary}. Errors are quoted at 1~$\sigma$ level throughout the paper.

\begin{table}
\vspace{-0.in}
\begin{center}
\caption{Parameters of NGC~5908.}
\footnotesize
\begin{tabular}{lcccccccccccccc}
\hline\hline
Parameters & Value & Reference \\
\hline
Type & SA(s)b & 1 \\
Distance & 51.9 Mpc & 1 \\
redshift & 0.011028 & 1 \\
scale & $1^{\prime\prime}=0.252\rm~kpc$ & 1 \\
inclination & $65.31^\circ$ & 2 \\
$v_{\rm rot}$ & $347\rm~km~s^{-1}$ & 3 \\
$M_{\rm HI}$ & $5.9\times10^9\rm~M_\odot$ & 4 \\
$M_*$ & $2.56_{-0.15}^{+0.02}\times10^{11}\rm~M_\odot$ & 6 \\
SFR & $3.81\pm0.09\rm~M_\odot~yr^{-1}$ & 6 \\
$M_{\rm 200}$ & $8.1\times10^{12}\rm~M_\odot$ & 5 \\
$r_{\rm 200}$ & 417~kpc & 5 \\
$kT$ & $0.38_{-0.09}^{+0.64}\rm~keV$ & 5,6 \\
$L_{\rm X,r<0.1r_{200}}$ & $7.2_{-2.3}^{+2.9}\times10^{39}\rm~ergs~s^{-1}$ & 5,6 \\
$r_{\rm cool}$ & $13.9_{-6.4}^{+4.9}\rm~kpc$ & 5,6 \\
$\dot{M}_{\rm cool,r<r_{cool}}$ & $0.37(<1.55)\rm~M_\odot~yr^{-1}$ & 5,6 \\
$M_{\rm hot,r<r_{200}}$ & $1.4_{-0.6}^{+3.3}\times10^{10}f^{1/2}\rm~M_\odot$ & 5,6 \\
\hline
$M_{\rm H_2,^{12}CO}$ & $(8.3\pm0.4)\times10^9\rm~M_\odot$ & 7 \\
$M_{\rm H_2,^{13}CO}$ & $(5.2\pm0.4)\times10^9\rm~M_\odot$ & 7 \\
$M_{\rm H_2,average}$ & $(6.8\pm1.7)\times10^9\rm~M_\odot$ & 7 \\
$\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 10}}{^{13}CO_{\rm 10}}}},median}$ & $7.0\pm1.7$ & 7 \\
$\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 21}}{^{12}CO_{\rm 10}}}},median}$ & $0.43\pm0.11$ & 7 \\
$\tau_{\rm ^{13}CO,median}$ & $0.16\pm0.03$ & 7 \\
$T_{\rm K,median}$ & $32\pm9\rm~K$ & 7 \\
$M_{\rm vir}$ & $(1.4\pm0.1)\times10^{12}\rm~M_\odot$ & 7 \\
$\Sigma_{\rm H_2}$ & $5.4\pm1.4\rm~M_\odot~pc^{-2}$ & 7 \\
$\Sigma_{\rm H_2+HI}$ & $10.1\pm1.4\rm~M_\odot~pc^{-2}$ & 7 \\
\hline\hline
\end{tabular}\label{table:NGC5908}
\end{center}
$v_{\rm rot}$ and $M_{\rm HI}$ are the inclination corrected rotation velocity and the atomic hydrogren mass obtained from the \ion{H}{1} 21-cm line observations. $M_*$ is the stellar mass estimated from the K-band magnitude. SFR is the star formation rate estimated from the \emph{WISE} $22\rm~\mu m$ data. $M_{\rm 200}$ is the dark matter halo mass (with density 200 times of the critical density of the Universe) estimated from $v_{\rm rot}$ with the NFW model (\citealt{Navarro96}). $r_{\rm 200}$ is the radius of the dark matter halo. $kT$ is the hot gas temperature. $L_{\rm X,r<0.1r_{200}}$ is the 0.5-2~keV soft X-ray luminosity of the hot gas component measured within $0.1r_{\rm 200}$. $r_{\rm cool}$ is the cooling radius defined as where the radiative cooling timescale equals to 10~Gyr. $\dot{M}_{\rm cool,r<r_{cool}}$ is the integrated radiative cooling rate calculated within $r_{\rm cool}$. $M_{\rm hot,r<r_{200}}$ is the total hot gas mass within $r_{\rm 200}$. All the hot gas parameters are estimated based on \emph{XMM-Newton} observations \citep{Li16b,Li17}. $M_{\rm H_2,^{12}CO}$ and $M_{\rm H_2,^{13}CO}$ are the molecular gas mass measured from the $^{12}$CO and $^{13}$CO~$J=1-0$ lines, respectively, while $M_{\rm H_2,average}$ is the average value of them. $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 10}}{^{13}CO_{\rm 10}}}},median}$, $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 21}}{^{12}CO_{\rm 10}}}},median}$, $\tau_{\rm ^{13}CO,median}$, $T_{\rm K,median}$ are the median values of the $^{12}$CO~$J=1-0$ to $^{13}$CO~$J=1-0$ ratio, the $^{12}$CO~$J=2-1$ to $^{12}$CO~$J=1-0$ ratio, the optical depth of $^{13}$CO~$J=1-0$, and the kinetic temperature of the gas measured at different positions along the disk. $M_{\rm vir}$ is the virial mass of the dark matter halo measured from the CO line rotation curves. $\Sigma_{\rm H_2}$ and $\Sigma_{\rm H_2+HI}$ are the surface density of the molecular or total cold gas, assuming the radius of the cold gas disk is $20\rm~kpc$.\\

References in this table:\\
1. NED (\url{https://ned.ipac.caltech.edu})\\
2. HyperLeda (\url{http://leda.univ-lyon1.fr})\\
3. \citet{vanMoorsel82}\\
4. \citet{Springob05}\\
5. \citet{Li16b}\\
6. \citet{Li17}\\
7. This paper
\end{table}

\section{Data Reduction}\label{sec:datareduction}

The IRAM 30m observations of NGC~5908 was taken in 2016B (on July 26, 2016; Project ID 062-16; PI: Jiang-Tao Li) and 2018B semesters (on August 21, 2018; Project ID 063-18; PI: Jiang-Tao Li), respectively. The observations were taken with the Eight MIxer Receiver (EMIR) in Wobbler switching (WSW) mode in 2016B and in position switching (PSW) mode in 2018B, with the E90/E230 combination covering the CO $J=1-0$ and $J=2-1$ lines simultaneously. The fast Fourier transform spectrometer (FTS) backend was used, which provides a frequency resolution of $200\rm~kHz$. The half power beam width (HPBW) of IRAM 30m is $\sim10.7^{\prime\prime}$ at 230~GHz and $21.3^{\prime\prime}$ at 115~GHz. The 2016B observations were taken from eight positions along the dustlane of this highly inclined disk galaxy (Fig.~\ref{fig:IRAMbeam}). For the inner regions (white solid circles in Fig.~\ref{fig:IRAMbeam}), the exposure time is $30.6\rm~minutes$ for each position, while for the outermost regions at the edge of the dustlane (black solid circles in Fig.~\ref{fig:IRAMbeam}), we adopted $62\rm~minutes$ for each position to achieve a better sensitivity. We only observed two positions in the 2018B observations: the nuclear region (position ``8'' in Fig.~\ref{fig:IRAMbeam}) has an exposure time of $9.8\rm~minutes$, and the outer region at the edge of the dustlane (position ``9'' in Fig.~\ref{fig:IRAMbeam}) has an exposure time of $68.8\rm~minutes$. The 2018B observations did not cover the $^{13}$CO $J=1-0$ line at the redshift of NGC~5908.

\begin{figure}
\begin{center}
\epsfig{figure=NGC5908_imageFOV_4arcm_SDSSg_IRAM12CO10beam_b.eps,width=0.48\textwidth,angle=0, clip=}
\caption{SDSS r-band image of the central $4^\prime\times4^\prime$ region of NGC~5908. The circles are the location of the IRAM 30m beams with the size indicating the beam size at $^{12}$CO~$J=1-0$ band. The black solid circles have twice the exposure time as the white solid ones. The two dashed circles (``8'' and ``9'') are taken in the 2018B semester, with ``9'' has an exposure time comparable to the black solid circles while ``8'' has much shorter exposure time (see text for details). Most of the observations are along the dustlane, except for position ``8'' which is on the galactic center and slightly offset from the dustlane. The scale bar has a length of 20~kpc assuming a distance of $d=51.9\rm~Mpc$.
}\label{fig:IRAMbeam}
\end{center}
\end{figure}

$^{12}$CO~$J=1-0$ (rest frame frequency $\nu_{\rm rest}=115.271\rm~GHz$; Fig.~\ref{fig:12CO10spec}), $^{12}$CO~$J=2-1$ ($\nu_{\rm rest}=230.538\rm~GHz$; Fig.~\ref{fig:12CO21spec}), and $^{13}$CO~$J=1-0$ lines ($\nu_{\rm rest}=110.201\rm~GHz$; Fig.~\ref{fig:13CO10spec}) have been detected at most of the positions (except for $^{13}$CO~$J=1-0$ at region~7 and the two positions 8 and 9 observed in 2018B) around the redshift of the galaxy. The velocity resolution was typically rebinned to $(10-20)\rm~km~s^{-1}$ to detect and well resolve the emission lines.

We calibrate and reduce the data following the standard steps with the GILDAS/CLASS package (\url{http://www.iram.fr/IRAMFR/GILDAS}; \citealt{Pety05}). The flux was calibrated during the observations using the standard sources. We correct the integrated line intensity ($I$, in unit of $\rm K~km~s^{-1}$, integrate the antenna temperature over a given velocity range) with the main beam efficiency using the recommended value of $B_{\rm eff}=78\%$ at 115~GHz for the $J=1-0$ transitions and 59\% at 230~GHz for the $J=2-1$ transition on the IRAM website (\url{http://www.iram.es/IRAMES/mainWiki/Iram30mEfficiencies}). We also adopt the recommended forward efficiencies of $F_{\rm eff}=94\%$ at 115~GHz for the $J=1-0$ transitions and 92\% at 230~GHz for the $J=2-1$ transition from the same website.

The emission lines are fitted with either a 1-gauss or 2-gauss model plus a linear baseline determined typically at $|v|<1400\rm~km~s^{-1}$ from the systematic velocity of the galaxy. The frequency windows used to fit the baseline are determined manually for each spectrum (windows are not plotted in Figs.~\ref{fig:12CO10spec}, \ref{fig:12CO21spec}, \ref{fig:13CO10spec}), after masking channels covering the emission lines or with significantly non-linear baselines (e.g., $v\lesssim-500\rm~km~s^{-1}$ in position-8 of Fig.~\ref{fig:12CO10spec}, $v\gtrsim400\rm~km~s^{-1}$ in position-9 of Fig.~\ref{fig:12CO21spec}, $|v|\gtrsim1000\rm~km~s^{-1}$ in position-6 of Fig.~\ref{fig:13CO10spec}, etc.). The number of gaussian lines used in the fit is determined by whether or not the data can be well fitted with a single gaussian model. In many regions, in addition to a broad component with a typical line width of $(100-400)\rm~km~s^{-1}$, there is often an additional narrow component with a line width of a few tens of $\rm~km~s^{-1}$. This decomposition may lead to the larger errors of some parameters measured in the inner region of the galaxy (e.g., Fig.~\ref{fig:LineAreaProfile}). In other regions, however, a single broad or narrow component can fit the data well.

The broad and narrow components are often significantly shifted from each other. We therefore calculate an average line velocity by weighting the two components with their velocity integrated intensity. This averaged line velocity $v$ will be used to construct rotation curves in \S\ref{subsec:rotationcurve}. All these directly measured parameters are summarized in Table~\ref{table:COlinepara}. The corrected integrated line intensities are presented in Fig.~\ref{fig:LineAreaProfile}, while the rotation curves constructed with the averaged line velocities will be discussed in \S\ref{subsec:rotationcurve}. We do not list the width of the CO lines, which is not directly used in the paper, and in some cases largely affected by the decomposing of different components. In general, the largest width of the broad component around the center of the galaxy is $\sim400\rm~km~s^{-1}$ (Figs.~\ref{fig:12CO10spec}, \ref{fig:12CO21spec}, \ref{fig:13CO10spec}). If the line is dynamically broadened, such a large line width indicates a deep gravitational potential, as will be discussed in \S\ref{subsec:rotationcurve}.

\begin{figure*}
\begin{center}
\epsfig{figure=NGC5908_LineAreaProfile.eps,width=1.0\textwidth,angle=0, clip=}
\caption{The main beam and forward efficiency corrected integrated line intensity of $^{12}$CO~$J=1-0$ (a), $^{13}$CO~$J=1-0$ (b), and $^{12}$CO~$J=2-1$ (c) along the galactic disk. The x-axis is the distance along the galactic plane from the galactic center. The vertical line in each panel marks the location of the galactic center. We also convert the $^{12}$CO~$J=1-0$ and $^{13}$CO~$J=1-0$ intensity to the molecular gas column density $N_{\rm H_2}$ in (a) and (b).
}\label{fig:LineAreaProfile}
\end{center}
\end{figure*}

For the ratio between different emission lines, we need to correct for the different beam dilution at different frequencies. NGC~5908 has been observed in CO~$J=1-0$ by CARMA as part of the EDGE-CALIFA Survey \citep{Bolatto17}. The CO~$J=1-0$ emission in the inner region of the galactic disk (radial extension comparable to the dustlane) is resolved and typically smaller than the IRAM 30m beam size in the vertical direction. The projected molecular gas distribution in NGC~5908 is therefore neither a point-like source nor a 2-D extended source. We assume the distribution of the molecular gas in NGC~5908 is ``disk'' like, i.e., continuous along the galactic disk while less extended than the main beam size of IRAM 30m in the vertical direction, consistent with the CARMA CO~$J=1-0$ image. We then construct 1-D ``images'' of different CO lines from the isolated IRAM 30m pointings. These CO images have a vertical extension equal to the size of the IRAM main beam at the corresponding frequencies. As we have chosen a separation of different pointings to be roughly equal to the IRAM main beam size at the CO~$J=2-1$ line, the intensity distributions along the galactic disk at all the frequencies of interest are continuous. We then convolve the higher frequency line images to the same resolution as the lower frequency ones when calculating their ratios. Compared to the directly measured line ratios, the measured beam dilution correction factor for the $^{12}$CO~$J=1-0$/$^{13}$CO~$J=1-0$ ratio is typically 0.87-0.95, while it is typically 0.38-0.65 for the $^{12}$CO~$J=2-1$/$^{12}$CO~$J=1-0$ ratio. The corrected line ratios are listed in Table~\ref{table:COlinepara} and plotted against the radial distance in Fig.~\ref{fig:RatioProfile}.

\begin{figure*}
\begin{center}
\epsfig{figure=NGC5908_RatioProfile.eps,width=1.0\textwidth,angle=0, clip=}
\caption{(a) $^{12}$CO~$J=1-0$/$^{13}$CO~$J=1-0$ line ratio. (b) $^{12}$CO~$J=2-1$/$^{12}$CO~$J=1-0$ line ratio. Both line ratios have been corrected for beam dilution. The x-axis is the distance along the galactic plane from the galactic center.}\label{fig:RatioProfile}
\end{center}
\end{figure*}

\section{Results and Discussion}\label{sec:resultsdiscussion}

\subsection{Column density distribution and total mass of molecular gas}\label{subsec:IntensityNH2}

We first derive the molecular gas column density $N_{\rm H_2}$ from the main beam and forward efficiency corrected, integrated CO line intensity $I_{\rm CO}$ using the conversion factor defined as $X\equiv N_{\rm H_2}/I_{\rm CO}$, where $N_{\rm H_2}$ is in unit of $10^{21}\rm~cm^{-2}$ and $I_{\rm CO}$ is in unit of $\rm K~km~s^{-1}$. Both the ${\rm ^{12}CO}$ and ${\rm ^{13}CO}$~$J=1-0$ lines can be used to measure $N_{\rm H_2}$, but the conversion factor $X$ has large systematic uncertainties. We adopt an empirical $X_{{\rm ^{12}CO}~J=1-0}=0.2\times10^{21}\rm~cm^{-2}/(K~km~s^{-1})$ (e.g., \citealt{Nishiyama01,Shetty11,Bolatto13}), which however, may be highly variable in extreme physical conditions and is often underestimated with only low-$J$ CO transitions (e.g., \citealt{Papadopoulos12b}). The $^{12}$CO~$J=1-0$ line, owing to the high abundance of ${\rm ^{12}C}$, may be highly affected by the optical depth effect. On the other hand, the abundance of ${\rm ^{13}CO}$ and the physical state of molecular gas (in diffuse or dense clouds) both show significant variations across the disk of many nearby galaxies, resulting in a ${\rm ^{13}CO}$-to-$N_{\rm H_2}$ conversion factor $X_{{\rm ^{13}CO}~J=1-0}=1.0\times10^{21}\rm~cm^{-2}/(K~km~s^{-1})$ with a standard deviation of a factor of two (e.g., \citealt{Cormier18}].
In general, it is often suggested that $X_{\rm CO}$ decreases with increasing metallicity (e.g., \citealt{Schruba12}). A lower $X_{\rm CO}$ is also found in starburst galaxies or in the central bright regions with high stellar surface density in some galaxies (see a review in \citealt{Bolatto13}). However, none of these processes seem to highly affect the $X_{\rm CO}$ in a massive non-starburst galaxy such as NGC~5908. In this paper, we present $N_{\rm H_2}$ measured from both the ${\rm ^{12}CO}$ and ${\rm ^{13}CO}$~$J=1-0$ lines with the conversion factors of $X_{{\rm ^{12}CO}~J=1-0}=0.2\times10^{21}\rm~cm^{-2}/(K~km~s^{-1})$ and $X_{{\rm ^{13}CO}~J=1-0}=1.0\times10^{21}\rm~cm^{-2}/(K~km~s^{-1})$. The results are summarized in Table~\ref{table:COlinepara}.

Radial distribution of $N_{\rm H_2}$ as derived above is plotted together with the integrated intensities of the $^{12}$CO~$J=1-0$, $^{13}$CO~$J=1-0$, and $^{12}$CO~$J=2-1$ lines in Fig.~\ref{fig:LineAreaProfile}. We caution that the derived $N_{\rm H_2}$ depends on the filling factor $f$ of the CO emission region within the beam as $f^{-1}$. In highly inclined galaxies with most of the molecular gas distributed within a thin disk, the apparent vertical thickness of the molecular disk may be smaller than the IRAM 30m beam size (supported by the spatially resolved $^{12}$CO~$J=1-0$ image from \citealt{Bolatto17}), and $f$ may be significantly less than 1, so the derived $N_{\rm H_2}$ may just represent a lower limit of the real molecular gas column density.

Integrating the $N_{\rm H_2}$ profile and assuming the vertical extension of the molecular gas disk equals to the main beam size of IRAM 30m at the corresponding frequencies, we can obtain the total molecular gas mass of NGC~5908 to be $M_{\rm H_2}=8.26\pm0.35\times10^{9}\rm~M_\odot$ ($5.16\pm0.42\times10^{9}\rm~M_\odot$) based on ${\rm ^{12}CO}~J=1-0$ (${\rm ^{13}CO}~J=1-0$). Since $N_{\rm H_2}$ adopted in calculating $M_{\rm H_2}$ is an average value within the beam, this derived $M_{\rm H_2}$ does \emph{not} depend on the filling factor $f$.

\subsection{CO line ratios and physical conditions of molecular gas}\label{subsec:RatioPara}

$^{12}$CO~$J=1-0$, $J=2-1$, and $^{13}$CO~$J=1-0$ emission lines are clearly identified in most of the positions. Their integrated intensity ratios are quite informative of the physical conditions of the molecular gas in the galaxy. In this section, we present the $^{12}$CO/$^{13}$CO~$J=1-0$ and $^{12}$CO~$J=2-1$/$J=1-0$ line ratios (Fig.~\ref{fig:RatioProfile}) and some physical parameters derived from them (Fig.~\ref{fig:ParaProfile}; the parameters are summarized in Table~\ref{table:COlinepara}), after correcting the beam dilution at the corresponding line frequencies following the procedure described in \S\ref{sec:datareduction}.

The $^{12}$CO/$^{13}$CO line ratio is basically affected by two factors: the abundance of $^{13}$CO and the optical depth of the CO lines (e.g., \citealt{Alatalo15,JimenezDonaire17}). $^{13}$CO is preferentially formed in cold regions via ion-molecule interaction. This isotope-dependent fractionation will increase the $^{12}$CO/$^{13}$CO abundance ratio in warm molecular clouds. Furthermore, $^{13}$C is only produced by the CN cycle of Helium Burning in intermediate-mass stars, or as a secondary product in low-mass and high-mass ($>10\rm~M_\odot$) stars \citep{Sage91}. The total effect related to molecular abundance is thus a higher $^{12}$CO/$^{13}$CO abundance ratio in recent star forming regions (e.g., \citealt{JimenezDonaire17,Sliwa17a}).
On the other hand, the $^{12}$CO/$^{13}$CO line ratio could also be affected by the optical depth effects, which may either be caused by the change of gas temperature/density or by the presence of a diffuse, non-self-gravitating gas phase. These optical depth effects may result in the higher $^{12}$CO/$^{13}$CO line ratio in extensive star forming galaxies (e.g., \citealt{Tan11,JimenezDonaire17,Cormier18}). This is often explained as that $^{12}$CO emission largely arises from a warm diffuse inter-clumpy medium whereas $^{13}$CO emission mainly originates in denser cores. In active star forming regions, strong UV emission, SN shocks, and cosmic rays may heat, perturb, and dissociate the molecular cloud, resulting in a more significant decrease of the optical depth of the $^{12}$CO-rich envelope (than the $^{13}$CO-rich core). There are thus more $^{12}$CO photons escaping out of the molecular clouds, producing higher $^{12}$CO/$^{13}$CO line ratios. The $^{12}$CO/$^{13}$CO line ratios measured in NGC~5908 (with a median value of $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 10}}{^{13}CO_{\rm 10}}}}}=7.0\pm1.7$; Table~\ref{table:COlinepara}) is in general comparable to some non-star-forming or normal star forming galaxies, but not as high as extreme starburst galaxies (e.g., \citealt{Tan11,Alatalo15,Sliwa17a,Sliwa17b,Cormier18}). Furthermore, $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 10}}{^{13}CO_{\rm 10}}}}}$ does not increase in the nuclear region (Fig.~\ref{fig:RatioProfile}a). We therefore believe the $^{12}$CO/$^{13}$CO line ratio in NGC~5908 is not significantly affected by star formation feedback.

The $^{12}$CO~$J=2-1$/$J=1-0$ line ratio depends on the temperature and optical depth, thus the structure and heating sources of the molecular clouds. Based on the $^{12}$CO~$J=2-1$/$J=1-0$ line ratio, most of the Galactic molecular clouds could often be classified into two types: the low ratio gas with $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 21}}{^{12}CO_{\rm 10}}}}}<0.7$ and the high ratio gas with $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 21}}{^{12}CO_{\rm 10}}}}}=0.7-1.0$ \citep{Hasegawa97}. The low ratio gas is thought to be in molecular clumps with extended envelopes, where the CO emission mostly comes from low-density gas. On the other hand, the high ratio gas is in highly confined clumps with a steep density gradient and a thin CO emitting envelope, and is thus often found in the bright ridges of molecular clouds which are associated with star formation regions but not directly related to massive star formation (the low and high ratio gas is in general found in molecular clouds with a density $\lesssim10^2\rm~cm^{-3}$ or $\gtrsim10^2\rm~cm^{-3}$; e.g., \citealt{Penaloza17}). There is also another phase of molecular gas with $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 21}}{^{12}CO_{\rm 10}}}}}>1$ (very high ratio gas). These gas clouds are influenced by significant external heating by UV photons from young stars or shock from SNe, both closely related to active star formation (e.g., \citealt{Hasegawa97}).

The CO line ratios is in general highly affected by the local environmental conditions, such as the supersonic turbulence of the molecular clouds, the interstellar radiation field, and the cosmic ray ionization rate, etc. (e.g., \citealt{Penaloza18}). In most of the cases, efficient heating via these processes are only important in extreme starburst environments (e.g., \citealt{Papadopoulos12a}), although some molecular clouds with $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 21}}{^{12}CO_{\rm 10}}}}}>1$ have also been suggested to be mainly heated by background cosmic rays (e.g., \citealt{Zhou18}). In most of the regions (except for the outermost regions with large error bars), the observed $^{12}$CO~$J=2-1$/$J=1-0$ line ratio in NGC~5908 is $<0.7$, with a median value of $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 21}}{^{12}CO_{\rm 10}}}}}=0.43\pm0.11$ (Table~\ref{table:COlinepara}). Furthermore, we do not find any significant increase of $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 21}}{^{12}CO_{\rm 10}}}}}$ in the nuclear region where the star formation is often the strongest in spiral galaxies. Therefore, we conclude that star formation in NGC~5908 is not intensive enough to modify $\mathcal{R}_{\rm \mathsmaller{\mathsmaller{\frac{^{12}CO_{\rm 21}}{^{12}CO_{\rm 10}}}}}$. However, we notice that there is a prominent $^{12}$CO~$J=2-1$ narrow line detected in the nuclear region (position ``0'' in Fig.~\ref{fig:12CO21spec}), but no corresponding component is detected in the $^{12}$CO~$J=1-0$ and $^{13}$CO~$J=1-0$ bands (Figs.~\ref{fig:12CO10spec}, \ref{fig:13CO10spec}, Table~\ref{table:COlinepara}), indicating the presence of some external heating sources. Either weak star formation or the AGN \citep{Li16b} may contribute in the heating of the molecular clouds in the nuclear region.

We next roughly estimate some derived physical parameters based on a few assumptions: (1) the molecular cloud is under the local thermal equilibrium (LTE) condition; (2) the emission lines from different CO isotopologues are co-spatial and have the same filling factor within the telescope beam, they also have the same excitation temperature; (3) the $^{13}$CO~$J=1-0$ line is optically thin while the $^{12}$CO~$J=1-0$ line is optically thick. All the assumptions need to be confirmed but are in general true for a regular galaxy with no extreme conditions. Under these assumptions, the optical depth of $^{13}$CO $\tau_{\rm ^{13}CO}$ can be derived from the $^{12}$CO/$^{13}$CO line ratio \citep{Tan11}:
\begin{equation}\label{equi:tau13CO}
\tau_{\rm ^{13}CO}=\ln[(1-\frac{I_{\rm ^{13}CO~J=1-0}}{I_{\rm ^{12}CO~J=1-0}})^{-1}].
\end{equation}
The derived $\tau_{\rm ^{13}CO}$ is listed in Table~\ref{table:COlinepara} and plotted in Fig.~\ref{fig:ParaProfile}a. $\tau_{\rm ^{13}CO}$ is $\lesssim0.2$ throughout the disk, with a median value of $0.16\pm0.03$.

\begin{figure*}
\begin{center}
\epsfig{figure=NGC5908_ParaProfile.eps,width=1.0\textwidth,angle=0, clip=}
\caption{(a) Optical depth of $^{13}$CO ($\tau_{\rm ^{13}CO}$). (b) Kinetic temperature ($T_{\rm K}$) of the molecular gas under the LTE assumption. The x-axis is the distance along the galactic plane from the galactic center.}\label{fig:ParaProfile}
\end{center}
\end{figure*}

The temperature of the molecular cloud could be estimated from the relative strength of the $^{12}$CO and $^{13}$CO lines. $N_{\rm H_2}$ can also be derived from the $^{13}$CO~$J=1-0$ line as \citep{Tan11}:
\begin{equation}\label{equi:NH213CO}
N_{\rm H_2}/{\rm cm^{-2}}=2.25\times10^{20}[\frac{\tau_{\rm ^{13}CO}}{1-e^{-\tau_{\rm ^{13}CO}}}]\frac{I_{\rm ^{13}CO~J=1-0}}{1-e^{-5.29/T_{\rm ex}}}
\end{equation}
where the $^{13}$CO abundance ${\rm [^{13}CO]/[H_2]}$ is taken to be $8\times10^{-5}/60$ \citep{Frerking82}. We also estimate the kinetic temperature of the gas $T_{\rm K}$ by equating Eq.~\ref{equi:NH213CO} to the $N_{\rm H_2}$ derived from $I_{{\rm ^{12}CO}~J=1-0}$. The derived $T_{\rm K}$ is listed in Table~\ref{table:COlinepara} and plotted in Fig.~\ref{fig:ParaProfile}b, with a median value of $32\pm9\rm~K$. At $r\lesssim8\rm~kpc$, $T_{\rm K}$ is quite stable at a value comparable to the median value, but $T_{\rm K}$ shows large uncertainty and fluctuation at larger radii. In interstellar molecular clouds without significant external heating sources, $T_{\rm K}$ is often $<20\rm~K$, so there could be moderate heating of the molecular clouds in NGC~5908, but the relatively low $T_{\rm K}$ compared to $\sim10^2\rm~K$ in starburst galaxies (e.g., \citealt{Tan11}) rules out a significant external heating by active star forming processes.

\subsection{Molecular gas rotation curve}\label{subsec:rotationcurve}

IRAM 30m observations of the molecular lines provide higher velocity resolution than any other gas components to study the fine structure of gas dynamics. The almost edge-on orientation of NGC~5908 is also optimized to study the rotation curve of this extremely massive spiral galaxy with least uncertainty on the inclination correction.

\begin{figure}
\begin{center}
\epsfig{figure=NGC5908_CO_VelocityProfile.eps,width=0.5\textwidth,angle=0, clip=}
\caption{Rotation curves of the $^{12}$CO~$J=1-0$ (diamond), $^{13}$CO~$J=1-0$ (triangle), and $^{12}$CO~$J=2-1$ (box) lines along the galactic disk. The x-axis is the distance along the galactic plane from the galactic center. Data points of the $^{13}$CO~$J=1-0$ and $^{12}$CO~$J=2-1$ lines are slightly shifted in the x-direction in order to avoid overlapping. The dotted vertical and horizontal lines show the best-fit shift from the optical center ($+0.8\rm~kpc$) and the systematic velocity of NGC~5908 ($+48\rm~km~s^{-1}$). The best-fit inclination angle is $89.98^\circ$, significantly larger than the value determined in optical ($65.31^\circ$, obtained from HyperLeda \citealt{Makarov14}). The solid curve is the universal rotation curve \citep{Salucci07} with a best-fit halo mass of $\log (M_{\rm vir}/M_\odot)=1.4\times10^{13}\rm~M_\odot$. The halo and disk components are plotted as the dashed and dash-dotted curves (very close to the solid curve), respectively.}\label{fig:rotationcurve}
\end{center}
\end{figure}

We combine the rotation curves of the $^{12}$CO~$J=1-0$, $^{13}$CO~$J=1-0$, and $^{12}$CO~$J=2-1$ lines in Fig.~\ref{fig:rotationcurve}. The average velocities of the lines and their errors, however, are measured based on averaging different components of the lines, as detailed in \S\ref{sec:datareduction}. At least at the outermost data points, we clearly see the trend of flattening of the rotation curves from the $^{12}$CO~$J=1-0$ and $J=2-1$ lines ($^{13}$CO~$J=1-0$ is not detected or covered), so the rotation curves could be used to estimate the dark matter halo mass of the galaxy (e.g., \citealt{Sofue01}).

We use the universal rotation curve of spiral galaxies from \citet{Salucci07} to characterize the shape of the rotation curves measured from the molecular lines. This universal rotation curve has two components: a stellar disk described by the Freeman disk \citep{Freeman70} and a dark matter halo described by the Burkert profile \citep{Burkert95} which converges to the NFW profile \citep{Navarro96} at large radii and often better fit the observed rotation curves. The universal rotation curve is thought to be valid out to the virial radius and has the virial mass of the dark matter halo ($M_{\rm vir}$) as the only galaxy indicator. With the inclination angle fixed at $i=65.31^\circ$ inferred from the optical morphology of the galaxy (obtained from HyperLeda; \citealt{Makarov14}), we cannot well fit the molecular line rotation curves ($\chi^2=383$ for a degree of freedom of $\rm d.o.f.=24$). We also notice that some authors have adopted a higher inclination angle of NGC~5908 (e.g., $i=81^\circ$ in \citealt{Kalinova17}). Therefore, we set it free and obtain a best-fit value of $i=(89.98_{-2.33}^{+2.36})^\circ$ (with a significantly reduced $\chi^2=145$ for $\rm d.o.f.=23$), indicating a perfectly edge-on molecular gas disk which may be slightly misaligned with the stellar disk. The best-fit virial mass of the dark matter halo is $M_{\rm vir}=1.42_{-0.08}^{+0.09}\times10^{13}\rm~M_{\rm \odot}$, roughly consistent with what is obtained in \citet{Li16b} ($M_{\rm 200}=8.1\times10^{12}\rm~M_\odot$) based on the \ion{H}{1} 21-cm line measurement (with a maximum rotation velocity of $347\rm~km~s^{-1}$, \citealt{vanMoorsel82}; consistent with our CO line measurement, Fig.~\ref{fig:rotationcurve}), considering the large systematical uncertainties in both model and measurement.

The above estimate of the dark matter halo mass based on the CO rotation curve may have large systematic uncertainties: (1) The peak of the universal rotation curve is always at $r\approx(10-20)\rm~kpc$ in a broad range of halo mass, within which the stellar component dominates \citep{Salucci07}. Without a good characterization at larger radii, the halo component cannot be directly constrained, especially for such massive galaxies whose dark matter distribution is very flat in the inner halo (the dashed curves in Fig.~\ref{fig:rotationcurve}). (2) For super-$L^\star$ galaxies as massive as NGC~5908, the stellar mass-halo mass relation may be quite different from those of lower mass galaxies (e.g., \citealt{Behroozi10}). Therefore, it may be problematic adopting $M_{\rm vir}$ as the only galaxy indicator. (3) \citet{Salucci07} does not include a bulge component in their rotation curve developed for spiral galaxies, while NGC~5908 has a significant bulge. (4) The back-reaction of baryons on the dark matter halo density distribution is not considered in the Burkert profile, and could make the radial distribution of dark matter significantly more concentrated (e.g., \citealt{Duffy10}), especially when the feedback is weak such as the case of NGC~5908 \citep{Li16b}. (5) NGC~5908 has a bright companion NGC~5905 located at $\approx200\rm~kpc$ away, whose tidal interaction may affect the dynamics of the gaseous disk. Considering these systematic uncertainties, we conclude that the dark matter halo mass of NGC~5908 is of the order of $\sim10^{13}\rm~M_{\rm \odot}$, one of the largest as a spiral galaxy. However, we emphasize that a more accurate measurement of $M_{\rm vir}$ requires better data and modeling. We will need a higher angular resolution and deeper CO line map to separate different overlaid velocity components and to detect gas at larger radii. We also need an updated analytical rotation curve including a bulge component and adopting the stellar mass-halo mass relation for super-$L^\star$ galaxies.

\subsection{How does cold gas affect the gas budget, star formation efficiency, and feedback efficiency?}\label{subsec:gasbudget}

In this section, we discuss how the measured cold gas properties help us to understand the evolution of this extremely massive, isolated spiral galaxy. We will compare the measured molecular gas content (plus the atomic gas mass obtained from archive) to the SFR, hot CGM radiative cooling rate ($\dot{M}_{\rm cool}$), and the expected baryon mass obtained from multi-wavelength observations. As the molecular gas mass estimated from both the ${\rm ^{12}CO}~J=1-0$ and ${\rm ^{13}CO}~J=1-0$ lines have significant systematic uncertainties, we adopt an average value of them ($M_{\rm H_2}=6.8\pm1.7\times10^{9}\rm~M_\odot$) in the following discussions. We also adopt an atomic hydrogen gas mass of $M_{\rm HI}=5.9\times10^{9}\rm~M_\odot$ from the \ion{H}{1} 21-cm line observations of \citet{vanMoorsel82}, so the total cold gas mass of NGC~5908 is $M_{\rm H_2+HI}\approx1.3\times10^{10}\rm~M_\odot$.

Galaxies in the local universe are observed to have the baryon content much lower than is needed in Big Bang nucleosynthesis, forming the ``missing baryon'' problem (e.g., \citealt{Bregman07,Bregman18,Li18}). The total mass of cold molecular and atomic gas of NGC~5908 is in general comparable to the mass contained in the extended hot CGM ($M_{\rm hot}=1.4_{-0.6}^{+3.3}\times10^{10}\rm~M_\odot$, Table~\ref{table:NGC5908}), so is important in the gas budget. However, compared to the stellar mass of $M_*=2.6\times10^{11}\rm~M_\odot$ and the expected total baryon mass of $\approx2\times10^{12}\rm~M_\odot$ from the estimated dark matter halo mass \citep{Li17}, the mass contained in the multi-phase gases is not quite important and far from accounting for the missing baryons.

The relatively small gas content, however, may still be important in the gas circulation and star formation of this massive, isolated, spiral galaxy.
We first check if the galaxy follows the Kennicutt-Schmidt law or not [$\Sigma_{\rm SFR}/{\rm M_\odot~yr^{-1}~kpc^{-2}}=(2.5\pm0.7)\times10^{-4}(\Sigma_{\rm H_2+HI}/{\rm M_\odot~pc^{-2}})^{1.4\pm0.15}$; \citealt{Kennicutt98}]. Assuming the radius of the star forming disk to be $r=20\rm~kpc$, consistent with the size of the dustlane and the detected CO lines (also see CARMA observations of the ${\rm ^{12}CO}~J=1-0$ line in \citealt{Bolatto17}), we can obtain the molecular gas surface density to be $\Sigma_{\rm H_2}=5.4\pm1.4\rm~M_\odot~pc^{-2}$, or the total cold gas surface density to be $\Sigma_{\rm H_2+HI}=10.1\pm1.4\rm~M_\odot~pc^{-2}$. Adopting the Kennicutt-Schmidt law, the expected SFR surface density would be $\Sigma_{\rm SFR,expect}=6.0_{-2.3}^{+3.3}\times10^{-3}\rm~M_\odot~yr^{-1}~kpc^{-2}$ (or $2.5_{-1.2}^{+1.7}\times10^{-3}\rm~M_\odot~yr^{-1}~kpc^{-2}$ if only considering the molecular gas traced by CO lines). Considering the large systematic uncertainties in the measurement of cold gas mass and the scatter of the Kennicutt-Schmidt law, this value is in general comparable to the measured $\Sigma_{\rm SFR}$ of $\approx3\times10^{-3}\rm~M_\odot~yr^{-1}~kpc^{-2}$ (\S\ref{sec:Introduction}; \citealt{Li16b}). We therefore do not find a significant suppression of star formation in NGC~5908, as often suggested in disk galaxies with a huge bulge due to some star formation quenching mechanisms such as morphological quenching (e.g., \citealt{Martig09,Li09,Li11}).

Accretion of the radiatively cooled hot halo gas may be an important source of cold gas observed in massive galaxies with an extensive hot CGM \citep{Li17,Li18}. Based on deep \emph{XMM-Newton} X-ray observations, we have measured the radiative cooling rate of a sample of massive spiral galaxies with the virial temperature high enough to produce virialized soft X-ray emitting gas, including NGC~5908 \citep{Li16b,Li17}. We obtained a cooling rate of the hot CGM within the cooling radius of $\dot{M}_{\rm cool}=0.37~(<1.55)\rm~M_\odot~yr^{-1}$ for NGC~5908, or the total cooled gas mass of $M_{\rm cool}<1.5\times10^{10}\rm~M_\odot$ within the Hubble time. The large uncertainty is caused by a fairly X-ray bright AGN (difficult to be cleanly removed from the \emph{XMM-Newton} image) which strongly affect the characterization of the radial distribution of hot gas in the inner halo. $\dot{M}_{\rm cool}$ is about one order of magnitude lower than the SFR, so in principle, even if all the cooled gas can be used for star formation, the accretion of the cooled hot CGM is still insufficient to compensate the gas consumed in star formation. It is not impossible to have other gas supplies such as the accretion of cool gas from the companion galaxy NGC~5905. However, the HI 21-cm line observation of NGC~5905/5908 did not show any signatures of gas transfer \citep{vanMoorsel82}. We therefore conclude that the cold gas observed in NGC~5908 is mostly leftover gas from previous starburst, instead of newly acquired from the very isolated environment.

Assuming the current SFR, it will need about ten times of the Hubble time to accumulate the huge stellar mass of NGC~5908. Therefore, the galaxy must be in a stage(s) before with much higher growth rate, either from mergers or starbursts. On the other hand, the SFR of NGC~5908 is relatively high among the CGM-MASS galaxies \citep{Li16b}, and is about one order of magnitude higher than that of M31 ($\sim0.4\rm~M_\odot~yr^{-1}$; \citealt{Barmby06}), another massive quiescent spiral galaxy in our close neighbourhood. Since there is no signature of recent triggering of star formation (such as galaxy merger, gas transfer, or enhanced cooling of the CGM etc.), we conclude that NGC~5908 is not completely quiescent, and it may be in the early stage after the previous starburst, before the star formation is completely extinguished and the ejected gas cools and falls back to the galaxy.

SN feedback is a key ingredient regulating the galaxy evolution. The thermalization efficiency, or the fraction of SN energy released as multi-wavelength emissions in the ISM or the CGM, is often only a few percent (e.g., \citealt{Li13b,Walch15}). Many factors may affect the thermalization efficiency (e.g., \citealt{Wang16}), which is poorly constrained directly from observations (e.g., \citealt{Strickland09}). A key factor which may affect the observed X-ray radiation efficiency (a good tracer of feedback or thermalization efficiency) is the cold-hot gas interaction, which is often expected to enhance the observed X-ray emission via many micro-processes at the interface of different gas phases (such as turbulent mixing, thermal evaporation, charge exchange, etc.; e.g., \citealt{Strickland02,Li13b,Zhang14}). NGC~5908 and most other CGM-MASS galaxies are among the spiral galaxies with the lowest X-ray radiation efficiency \citep{Li17}. However, unlike other CGM-MASS galaxies which are mostly poor in cool gas (Li J., et al., in prep.) so the low X-ray radiation efficiency is easily explained as the result of the lack of gas mixing (e.g., \citealt{Tang09}), NGC~5908 is quite rich in cool gas and is often expected to be relatively X-ray bright (e.g., \citealt{Li09,Li15}). The low X-ray radiation efficiency provides evidence that the previously internally ejected or externally accreted gas in the CGM is not yet cooled and well mixed with the cold gas.

\section{Summary and Conclusion}\label{sec:summary}

We present IRAM 30m observations of the $^{12}$CO~$J=1-0$, $^{12}$CO~$J=2-1$, and $^{13}$CO~$J=1-0$ lines from the highly inclined massive spiral galaxy NGC~5908 selected from the CGM-MASS sample. All these three lines have been detected in most of the positions along the galactic disk, except that $^{13}$CO~$J=1-0$ is not covered or clearly detected at the outermost positions. We model the lines with one or two gaussian components and calculate the integrated line intensities, line ratios, average velocity, and a few derived physical parameters. Below we summarize our major results and conclusions.

$\bullet$ The total mass of molecular gas in NGC~5908 estimated from the integrated $^{12}$CO~$J=1-0$ ($^{13}$CO~$J=1-0$) line intensity is $M_{\rm H_2}=8.3\pm0.4\times10^{9}\rm~M_\odot$ ($5.2\pm0.4\times10^{9}\rm~M_\odot$). Adding the atomic component measured with the \ion{H}{1} 21-cm line from the literature, the total cool gas mass is $\approx1.3\times10^{10}\rm~M_\odot$. The cool gas mass is thus comparable to the total mass of hot gas in the halo, so makes a significant contribution to the galaxy's gas budget, but is still far from sufficient to account for the ``missing baryons''.

$\bullet$ The rotation curves determined with a combination of different molecular lines significantly flatten at $r\approx15\rm~kpc$. Fitting the measured velocities of different molecular lines with the universal rotation curve from \citet{Salucci07} indicates that NGC~5908 has a dark matter halo with the mass of $M_{\rm vir}\sim10^{13}\rm~M_{\rm \odot}$. Although better data and modeling are required to accurately measure the halo mass, NGC~5908 is definitely among the most massive spiral galaxies yet known in the local universe. The basic scenario of gas cycling and star formation properties may thus be representative of a massive spiral galaxy evolved largely in isolation.

$\bullet$ The $^{12}$CO/$^{13}$CO~$J=1-0$ line ratio is in general comparable to normal star forming galaxies, but not as high as extremely starburst ones. It is thus likely that star formation feedback does not seriously affect the molecular gas properties. In the mean time, the $^{12}$CO~$J=2-1$/$J=1-0$ line ratio and the estimated gas temperature also indicate relatively weak star formation in this massive spiral galaxy. Comparison to the star formation law indicates that NGC~5908 is converting cool gas to young stars at a normal efficiency, with no significant suppression of star formation as often suggested in disk galaxies with a huge bulge. The radiative cooling of the hot CGM or any other external gas supply are probably insufficient to compensate the gas consumed in star formation. The galaxy must have a fast growth stage with mergers and/or starbursts in the past. It is probably now at an early stage after the starburst, with plenty of leftover cool gas, a relatively high SFR, low hot CGM cooling rate, and low X-ray emissivity.

\bigskip
\noindent\textbf{\uppercase{acknowledgements}}
\smallskip\\
\noindent The authors acknowledge Dr. Zhi-Yu Zhang and Dr. Qinghua Tan for helpful discussions. JTL and JNB acknowledge the financial support from NASA through the grants NNX15AM93G, SOF05-0020, 80NSSC18K0536, and NAS8-03060. PZ acknowledges the support from the NWO Veni Fellowship, grant no. 639.041.647 and NSFC grants 11503008 and 11590781. XJJ and YG are partially supported by National Key Basic Research and Development Program of China (Grant No. 2017YFA0402704), NSFC Grant No. 11420101002, and Chinese Academy of Sciences Key Research Program of Frontier Sciences (Grant No. QYZDJ-SSW-SLH008).

redpajama_set_name: RedPajamaArXiv


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The harm is that Goleman's self-promotion and unsupportable claims have served to trivialized the serious research which is being done by academic scientists.Deriving meaning in a time of chaos: The intersection between chaos engineering and observability.
Crystal Hirschorn discusses how organizations can benefit from combining established tech practices with incident planning, post-mortem-driven development, chaos engineering, and observability.
Pessimism is a mental attitude in which an undesirable outcome is anticipated from a given situation. Pessimists tend to focus on the negatives of life in general. A common question asked to test for pessimism is "Is the glass half empty or half full?"; in this situation a pessimist is said to see the glass as half empty, while an optimist is said to see the glass as half full.
PURPOSE STATEMENT The Searle Civil Justice Institute is a public policy institute devoted to producing timely, analytically rigorous, and balanced research on important civil justice issues confronting our free enterprise system.
A Critical Thinking Disposition Scale (CTDS) was developed.
Psychometric properties of the scale were tested. Two dimensions – Critical Openness and Reflective Scepticism – were identified. There was confirmatory support for the two-factor model in two different samples. Psychometric properties show the CTDS is a valid and reliable instrument.
Providing educators and students access to the highest quality practices and resources in reading and language arts instruction. But the philosophy that killed off truth proclaims unlimited tolerance for the 'language games' (i.e., opinions, beliefs and doctrines) that people find useful.
Effect of globalization on accounting practice and standard
Pedro and me
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An introduction to the issue of gun control and violence in the united states and canada
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Individual functions of public relations essay

redpajama_set_name: RedPajamaCommonCrawl


text:
William Byron Hillman
Changing the world, one word at a time…
ZEBRA'S ROCK and ME
The epic film ICE STATION ZEBRA started my career. As a very young actor working for the first time in a big budget studio film, I was cast as Rock Hudson's sidekick. The original role was to bring a comedy spirit into a very serious subject matter. After working 19 weeks on the old MGM Studio lot, I came away with filmmaking knowledge you couldn't buy in any college or film school.
Waiting in-between scenes, I roamed into the editing bay and watched Ferris Webster cut the film, drove the director John Sturges crazy looking over his shoulder and pestered the Producer John Calley until he gave me a production job to go along with my acting role.
Working with Rock Hudson, Ernie Borgnine, Jim Brown, Patrick McGoohan, Tony Bill, Lloyd Nolan and for a brief moment with Lawrence Harvey I gained a lifetime of knowledge in five short months.
Zebra's Rock and Me and just a snippet of the experience, from the long casting call, the interview, getting the job and then the learning process and a break that started a career.
© 2016 Bill Hillman Contact Me
Actor/Performer
Film/TV Director
Script Consultation
Mystery/Romance
Movie Stories
Music Associations
Product Spokesperson


Hire Antonio Villaraigosa to Speak at Events - Professional Speaker Booking Agency.
Antonio Villaraigosa is an American politician who served as the 41st Mayor of Los Angeles, California for almost 10 years. Prior to being elected Mayor he was a member of the California State Assembly for six years, the Democratic leader of the Assembly for two years, and the Speaker of the California State Assembly for two years. After leaving the State Assembly due to term limits he was elected to the Los Angeles City Council until he was elected Mayor a few years later. Villaraigosa is a member of the Democratic Party, and was national co-chairman of Hillary Clinton's presidential campaign, a member of President Barack Obama's Transition Economic Advisory Board, and Chairman of the Democratic National Convention in September 2012. He recently announced candidacy for Governor of California but came in third for primary election..
Learn how to hire Antonio Villaraigosa or research availability and pricing for booking Antonio Villaraigosa to speak at a corporate event, fundraiser, private party, social media campaign, fair or festival, tradeshow or conference, endorsement project, or hire Antonio Villaraigosa as a guest speaker, please submit the form to our agency.
Frequently Asked Questions about booking Antonio Villaraigosa.
Is Antonio Villaraigosa available to work my event?
Antonio Villaraigosa's current work schedule and location in relation to your event's type, date, budget, and locality will play a primary factor in the acceptance of booking Antonio Villaraigosa for your party. As long as your funding is commensurate to the price range to book Antonio Villaraigosa, CTI will propose your event to the official agency representing Antonio Villaraigosa. After we consult with them, we can circle back with you to provide a personal and accurate quote that includes: final costs, availability, and actual interest in being hired for your specific event or party.
How much is Antonio Villaraigosa charging for events?
CTI can give you the Antonio Villaraigosa booking price once we submit your event details to their camp. "How much does it cost to book Antonio Villaraigosa for an event?" is a frequent question we get, but the final Antonio Villaraigosa booking price is contingent on many variables and the booking fee we show is based on a range derived from our past experience with what will Antonio Villaraigosa charge for an event. Also, thier speaking fee might be different than the fee shown for the cost to perform or to just appear. Popularity, career stage, along with current demand will cause fluctuations in their speaking price too. The final booking price may be more than what is shown, but you should at least have a budget within that range for them to consider an appearance, performance or speaking engagement.
How do I contact the Antonio Villaraigosa agent or manager?
CTI negotiates on behalf of professional event planners and talent buyers for paid appearances! We cannot give out direct contact information of the Antonio Villaraigosa agent or help distribute fan mail, personal messages, gifts, requests for free appearances, or donations of time. The Antonio Villaraigosa manager and agent will only work with us if we present them with funded offers for their client to work your event.
Can I book Antonio Villaraigosa for an event at a price less than shown?
There is low probability to book Antonio Villaraigosa for a party with anything substantially less than the published booking cost price range. We will negotiate with the Antonio Villaraigosa agent on your behalf, but if your funding is not in place then it will more difficult to book Antonio Villaraigosa, because they get many offers to work events that are at or above asking price. It is also important to consider the travel costs when researching the Antonio Villaraigosa booking fee, as additional expenses like this, as well as an entourage of staff and equipment, are not necessarily built-in to the booking fee range shown. If your budget does not factor that in, then there is no benefit for them to want to be hired. We do not personally speak for Antonio Villaraigosa, but in our experience in booking talent for over 25 years, this is generally the outcome of inadequate funding.
CALL US TODAY (760) 729-2000 and speak with a CTI Antonio Villaraigosa booking agent to get direct availability and pricing for having this talent to work your event.
Contact us at (760) 729-2000 for complete details and information for the Antonio Villaraigosa speaking fee to appear as a guest speaker at a corporate event or other business speaking engagements like lectures, retreats and business summits.
With almost 30 years of industry experience working with professional event coordinators and buyers like you, we can successfully work to hire Antonio Villaraigosa to speak as a keynote speaker at conferences and tradeshows, or as a spokesperson for branding and promotional marketing, product or service launches, business projects, print advertising campaigns, media events, fundraisers, and even social marketing campaigns and guest appearances on TV/Movie specials including documentaries or infomercials.
CTI will directly contact the Antonio Villaraigosa agent, representative, or manager to present them with your event while inquiring about current availability and interest. If they want to work your event, then we begin pricing negotiations - on your behalf – to secure the lowest possible Antonio Villaraigosa booking fee they will accept. Let CTI be your speaker booking agency for Antonio Villaraigosa to hire them to give a speech at conventions, college and university commencements, trade shows, or charity events. The Antonio Villaraigosa booking price may dramatically change based on the location of spokesperson campaigns, speeches, concerts, or as a voice over on video games and television and radio commercials when considering domestic or international travel. CTI agency will help book Antonio Villaraigosa as a speaker if the buyer has the budget and if they are interested in the event. CTI can assist on the production needs for Antonio Villaraigosa when needed.


The world mapped out with every country's tourism slogan.
Yes, Jump Into Ireland is ours, apparently.
Posted in Design and tagged tagline, Tourism at 9:17 am on November 24, 2016 by Broadsheet.
always loved the poster in murray from flight of the conchords office – new zealand – why not?
"Jump into Ireland"? That's pants. When did that become the slogan?


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Breaking News: Aaron Brooks To Phoenix For Goran Dragic
by: Austin February 24, 2011
The reigning NBA Most Improved Player just became a backup. Again. Aaron Brook — who'd recently found himself stuck on the bench behind Kyle Lowry in Houston despite winning the Most Improved award last season while dropping 19 points per game and leading the NBA in three-pointers — has been traded to the Suns for Goran Dragic and Phoenix's (Lottery-protected) first-round draft pick.
Brooks is averaging 11.6 points and 3.8 assists, and his shooting percentages are way down from last year: 34% from the field, 28% beyond the arc. He missed several weeks with an ankle injury early in the season, and by the time he came back, Lowry had a stranglehold on the starting PG spot.
In Phoenix, Brooks will back up Steve Nash.
That used to be Dragic's job. After one breakout playoff game last spring, Dragic has been quiet this season. He's averaging 7.4 points and shooting just 27% from three-point range.
Tags: Aaron Brooks, DimeMag, GORAN DRAGIC, Houston Rockets, PHOENIX SUNS, Real Stories


This is the second time I've built this kit. I was far better prepared the second time around, lol. The first attempt a few years ago was well a very poor build.
I built this for a group build on a facebook page that I'm a member of. There is a contest, and I'm crossing my fingers, but won't know until January. Anywho I thought I would share some finished pics.
I did do some scratch building with this as well. I made the exhaust cover from a piece of cardboard, and tape for the handles. The intake cover is made from a piece of material coated in modge podge and shaped around the intake. The wheel chocks were made from a square piece of wooden dowel, which I filed to shape then painted. I put string on both sides so they would stay in place around the wheel. The static dischargers are just small pieces of stretched sprue glued in place and painted. I added some plumbing to the landing gear bays as well. Not entirely accurate, oh well.
Biggest gripe with this kit is the decals. They are fragile, and a bugger to get in place. Some didn't survive, and I had to paint some areas. I kind of wish I would of gotten masks, and painted everything on, but didn't think of it until after I already started with the decals.
Very nice, Keyda! The extra touches worked out well. Those markings are exactly why I never build Tbird a/c. If I ever do one, I'm building no.5, they apply the number inverted on the intake.
I think that turned out really nice. Really like the chocks. Nice job K!
Very nice work! Those decals look painful.
Those T-birds are very pretty and you certainly did justice to yours. Thanks for sharing.
Beautifully done Keyda. I built the same model and yes the decals where a tough go and like you , I had to paint/touch up several areas too.
I did mine in flight over the Daytona Speedway and intended to give the model to the pilots that inspired me to build it. I met all of them and had a nice chat. They where all well spoken and intelligent individuals and a tribute to our armed forces. But alas, after I got the plane built I never saw them again and the model remains on my shelf.
mississippivol, Thanks! Those decals nearly drove me mad, lol. I wanted to do the #5, but I went with the block 52 option which is what I saw this past summer, and that only allowed for the #1 jet marking wise. I wanted it to be accurate as far as the instructions this time around, the first time it was no where near accurate, lol.
Ole, They were, lol. That and the white paint.
Jay Jay, It was a nightmare. At one while during touch-ups I got blue paint on my finger somehow, and didn't notice. Well that turned into a nice blue smudge on the white paint. I managed to not freak out entirey and fixed it for the most part. I got to see them this year at our local airbase. I couldn't get near the planes, but my camera is a decent enough one where I could zoom in and at least get some reference photos. Still wish I could of done a walk around of the plane. I did use a few shots I found online.
Nice job Keyda, the plane looks great. Those decals do look like they would be a hassle, but end result looks fine. Nice touch adding the static wicks and the other scratch-built items. Good luck with the contest!
WOW!!! That is really nice. You did a spectacular job on that and deserve to win the contest. It's not easy pulling of clean shiny finishes but you killed it with this one. Well done.
MrStrecks, Thank you! The decals were the worst part, lol. I usually like doing decals cause it means I'm nearing completion, but these ones, ugh. Thanks!
BrandonK, Thanks! I learned not to use my normal primer when I'm painting the bird white, it took several coats to fully cover it. I swear I was going to go blind making sure it was evenly covered. I'm hoping to win the contest, I never win anything, lol. It was liked by a lot of people, so fingers crossed!
What primer did you use? Tamiya's Fine gray primer would have been great for a base coat, followed by their white primer. Works flawlessly for white paint.
I think it's Rustoleum to be honest, lol. It works great, and it's cheap, but it is a pretty dark shade of grey. Next time I paint anything white, I'll try something else, lol.
Spiffy job on a handsome fighter!
Looks really good K! Don't you just love applying those decals? You did great with such a PITA scheme which will require some type of touch ups here and there. Don't worry about the plumbing not being accurate as long as it looks busy in there. This is known as Gyzmology. Great idea about your covers.
plasticjunkie, I usually like decals, not in this case, lol. It was weird too, cause one side would go on great, then the other well not so much. I did have quite a few touch-ups to do, thankfully the paint matched the decals perfectly. I should of put more plumbing in there, but honestly using wire made it a bit of pain, and I should of used stretched sprue. Live and learn, it was my first time trying it. Thanks!
Stretched sprue is good. Lay it down get the shape you want then hit it with Tamiya thin and let it cook. When done, paint then apply a light wash to make the wires pop.
That's looking pretty tight. Nicely done.
I'll try that method next time, thanks!
I think this is one of your best so far. Just love that paint scheme!
Too bad the decals were a pain but you'd never know it.
Maximum effort was put into it that's for sure, lol. I have Tamiya's Skyray kit as well. I was going to pull that out of the stash, then looked at the decals and put it back in the stash, lol! I'm going to have to wait a while on that one!
.......I'm going to have to wait a while on that one!
You can handle it, you just don't know it.
Lol, I'm going to have to forget how much of a nightmare the decals were on this.
Kudos Keyda, you did great on such a challenging scheme.
You know how much I like the Thunderbirds and this looks awesome. Gloss is really hard to do and it shows well on your build! Whatever the hassles were with decals it doesn't seem to show. Nice lines on the blue coming around the nose, looks like every lined up and the spacing is uniform between stripes.
Thanks Mongoose! I thought about your build while I was doing this one, and really wished I would of purchased masks for painting the blue and red, lol. Despite all that it turned out a million times better than the first one I did!


text:
A Krasznoarmejszki járás () Oroszország egyik járása a Szaratovi területen. Székhelye Krasznoarmejszk.

Népesség
 1989-ben 23 404 lakosa volt.
 2002-ben 25 192 lakosa volt.
 2010-ben 48 739 lakosa volt, melyből 40 158 orosz, 848 kazah, 749 ukrán, 631 tatár, 554 német, 400 azeri, 310 örmény, 296 lezg, 229 fehérorosz, 184 csuvas, 175 csecsen, 160 mordvin, 89 tadzsik, 84 moldáv, 73 üzbég, 71 grúz, 57 mari, 56 koreai stb. Az adatok magukba foglalják a város lakosságát is.

Források
 Всероссийская перепись населения 2002 года. Национальный состав населения по регионам России. Демоскоп Weekly.
 A 2010-es népszámlálás adatai: http://www.gks.ru/free_doc/new_site/perepis2010/croc/perepis_itogi1612.htm

A Szaratovi terület járásai

redpajama_set_name: RedPajamaWikipedia


The EZ100 O-Rings are made to fit on all of our plastic bottles.
Orings should be replaced as needed or at the beginning of every milking season to prevent any loss of suction on your Udderly Ez Milker.
Not to be used with Glass Bottles. Call for replacements for that application.


text:
Our Schools - New Westminster School District
Welcome To New Westminster!
New Westminster School District has been providing a quality public education to its residents since the 1920's and the District consistently ranks among the top public boards in the province of British Columbia. From Kindergarten through to grade 12, New Westminster classrooms boast innovative learning and academic excellence as well as co-curricular opportunities for students. Many New Westminster graduates go on to study at top universities across Canada, the U.S.A, and countries around the world.
The New Westminster School District is committed to ensuring that its students become self assured and self sufficient adults who are wise, caring, creative and flexible and able to live successfully in an ever changing environment.
New Westminster School District Map
Download the School District Map
Organization of New Westminster School District
There are 12 schools in the District: eight elementary, three middle, and one secondary school. The District is currently in the process of planning a NEW! secondary school to replace the existing New Westminster Secondary School building which opened in 1955. The new building will be the largest project of its kind in the history of the Province.
Ages 5 – 10 Kindergarten – Grade 5* Connaught Heights
Lord Tweedsmuir
Qayqayt
F.W. Howay
Richard McBride
Queen Elizabeth *(K-4)
Ages 11 – 13 Grades 6 – 8* École Glenbrook Middle School
Fraser River Middle School
Queensborough Middle School* (Grades 5-8)
Ages 14 – 18 Grades 9 – 12 New Westminster Secondary
Highlights at New Westminster School District 40
Return t o School Plan
The New Westminster School District has been preparing for students to safely return to school from next Monday, January 10th. Please see the message from Superintendent Hachlaf explaining the measures taken for students to return to school. Please click "more" to be able to click on the message. more
Extension of Winter Break
The return of in-person learning will be delayed until January 10th to allow for enhanced safety measures. Please see the message from Superintendent Hachlaf for complete details. Please click "more" to be able to acces the link. more
Winter Vacation Office Hours
The International Education Office will be open 9:00 to 2:00 Monday, December 20th to Thursday, December 23rd. The office will be closed from Friday, December 24th and reopen with the return to school on Tuesday, January 4th. for student emergencies only please call 604.356.4980 or What's App at 604.802.7001. For all other inquiries please contact the international office at 604.517.6285 or email to iep@sd40.bc.ca. We wish everyone a very safe and happy holiday season and all the best for 2022. more


text:
XYZ Lab X workshop
La Scuola Open Source, Bari
We were given the opportunity to participate as teachers in the X laboratory. Two intense weeks (from 18th to 30th July) of laboratory within XYZ, to design the identity of The Open Source School, an "educational Institute, center of artistic and technological research and consultancy of Industry, Commerce and Crafts (both digital and non-digital)".
Together with some graphic design gurus – such as Giovanni Anceschi and Mauro Bubbico – some extremely talented professionals – such as Alessandro Tartaglia, Andrea Bergamini, Marco Goran Romano, Valerio Nicoletti and Giacomo Equizi – the special contribution of the processing ninja Danilo di Cuia and some very passionated students – like Michele Santella, Francesca Giorgio, Alessandra Rigano, Marco Laceranza, Gianluca Monaco, Giulia Cordin, Giacomo Boffo, Federica Salleri, Simona Zurlo, Giorgia Rocchi, Paola Sorrentino, Alberto Malossi, Alberto Gerin, Filippo Giannessi, Beatrice Bianchini, Paolo Musano, Federica di Toro, Chiara Santantonio, Francesco Brandi and Emma Magrini – we developed a visual system that defines a strong recognisable identity but at the same time leaves space for improvisation.An institutional system, but also a set of tools that can be taken and used by every member of the community around the school to gave its own interpretation.
Visual Concept
The key element of the identity is the composition of the logo. The four words are distributed on the four corners of the medium defining a white area where crazy things can happen. The idea is that the school itself, represented by the logo, it's a space where different people, experiences, ideas and projects can move freely. A place where the interaction in between all these elements contribute to generate meaning.
The words attached to the left and right side of the medium generate two visual axis where the rest of the contents can be placed, emphasising even more the white space.
We need to mention that the new identity was meant to question and replace the previous one. In order to make the community aware of the upcoming change and to test their reactions we have run a performance during the first week of workshop: the words "The Open Source Manifesto" where printed at the corners of an A4 paper and people were asked to freely draw a shape without covering the words. This performance gave away the identity to the people, making them able to do almost whatever they want with it. It was a first step in building a relation in between the new identity and the community that would have adopted it. At the same time worked as an inspiration for the possible shapes that could have been use to occupy the empty space.
Other Key Visuals Elements
Since the use of typography is the main element of this identity we have decided to design a new font. Starting from the HK Grotesk, released as Open Source, we have developed a new typeface: Freak. This new font includes some new freaky glyphs that give a stronger personality to the whole identity. The new font will be soon released as Open Source, becoming a fun to use tool for the whole community.
The colour palette features some very bright colours, inspired by the programming language and the hacker aesthetics. The idea is to replaced the ink within the yellow cartridge with a green flou one, which is also the reason why the other colours have no percentage of yellow in.
The last key element is the organic shape that would adapt to the space left by the typography. This represents the movement of the community acting within the school. It can be drawn by hands or automatically generated. This can be done with a ad-hoc Processing script that simulate the behaviour of a fluid interacting with the space occupied by typography.
Levels of use
This identity has been design in order to be used on three different levels:
A.Institutional communication
On the institutional material the identity only uses the typographic composition. With the four logo words attached to the corners and the typographical elements aligned to the axis corresponding to the two sides. The system is printed almost exclusively in black and white in order to be always easy and cheap to reproduce.
B. Promotional communication
The promotional material always includes one or more stains. On the promotional material about the school the stains are used in different shapes and colours in order to communicate the variety of the disciplines and activities offers by the school. On promotional material about one single course the stain's size is used to communicate the duration of the course, its colour stands for the theme while the contours distortion stands for the difficulty level.
C. Community's communication
Based on the result of the performance we already described, we decided to leave room for the free interpretation of the community members. People are free to use the space defined by the typography as they wish, following the only rule to don't cover the type. This approach have been tested again in a second performance where the participants were asked to fill the space on a shopper. The result is an immersive experience, where the community become user and producer getting involved in the definition of a living identity.
During the first week the whole group worked together in order to define the guidelines that would have driven the project.
In a first place the students were asked to identify the keywords that express the school. Then they were asked to take those keywords on a more abstract level – in order not to describe the school, but to evocate it – putting together an imagery that would have driven the design process. At the end they were also asked to make a collective visual research to start visualising their ideas and communicate them to the whole group.
All this initial phases were partially based on the p2p design strategies we've been developing during the past years. In particular the students were asked to work individually, to collect their input anonymously and to discuss all the proposals with the group. Trying not to push their own work, but to react on the others.
The materials collected in the research were organised in 4 principal concepts: Fluidity, Open Work, Freak and Materials. Based on these 4 directions the students gathered in small groups and eventually started to draw. They were asked to visualise one of those concept and to present them to the group, after the discussion they gathered in different groups in a way that everyone would have developed somebody else's work.
After this first process the students divided in three main groups, working like small design studios and corresponding to the three main output expected: the identity material, the website and the publishing. Due to the complexity of the project, the amount of people involved and the short time available most of the design was developed in parallel with a continuos exchange of proposals and solutions that would eventually converge to a single one saving room for discussion and personal interpretation.
The final result (available here) is a solid base for further development that demonstrates the effectiveness of the system proposed. It does still need some adjustments to be completed and actually used but on the other hand is meant from the beginning to be something that can be taken over by other designers and change during the time without losing its charm.
← Peer-2-peer graphic design workshop


Odell Brewing's latest year round release, Sippin' Pretty, is a ruby red, 4.5% ABV Fruited Sour brewed with a unique blend of super fruits and balanced with a touch of pink sea salt.
Sippin' Pretty gets it's bright color and fruit flavors from Brazilian guava and acai, mountain-grown elderberries, and pink sea salt from the Himalayas. The bright fruit flavors are complimented by a refreshing tartness and a lower ABV which creates a unique profile unlike anything else in Odell's portfolio.
"While we've always enjoyed brewing barrel-aged wild sours, we saw an opportunity brew something more thirst-quenching and sessionable with complex and interesting fruits," explains Head Brewer Bill Beymer.
Odell has spent the Summer tinkering with several fruited kettle-sours on their pilot systems in both Fort Collins and the new RiNo Brewhouse in Denver.
Sippin' Pretty presented a unique opportunity for Odell to explore flavor profiles that expand beyond the realm of traditional craft beer styles.
Sippin' Pretty's striking label art features a ruby-throated hummingbird in a lush scene of vibrant flowers and foliage. At first glance, the scene may look like a tropical jungle but the flora actually represents alpine wildflowers native to Colorado, such as the Columbine, Scarlet Gilia and Goldenrod.
Sippin' Pretty will be priced inline with core brands, available on draft and in 6-packs cans. The beer will debut in Larimer County on November 19th and be available throughout the rest of Odell's 18-state footprint by early December.


text:
Q: Recover Deleted Branch Git I have a huge issue that i need to solve (If it can be solved)
I have accidentally deleted a branch from local and from GitHub and would like to recover the work. However, where the problem lies is that I had not committed the work before it was deleted.
Is this still recoverable and how??
Cheers

redpajama_set_name: RedPajamaStackExchange