text:
\section{Introduction}

Water masers (H$_2$O; 22.23508\,GHz, ${6_{16} \rightarrow 5_{23}}$) and hydroxyl masers (OH; 1665\,MHz and 1667\,MHz) in the megamaser class have luminosities that far exceed their Galactic counterparts. They are best known as probes into some extreme environments such as merging galaxies, nuclear starbursts in molecular tori at 100\,pc scales in the case of OH, and AGN accretion disks at sub-pc scales, outflows, and the vicinity of jets in the case of H$_2$O. Water disk-masers are of particular interest and are found between an outer circumnuclear region of molecular gas that is too cold for maser excitation, and an inner atomic gas region that is too hot ($>8000$\,K) for the molecular gas phase. The kinematics and VLBI angular positions of disk- or torus-masers allow a well-constrained estimate of the central binding mass as in Mrk~273 \citep{2004AA...419..887K}, with more accurate mass estimates made with H$_2$O megamaser observations \citep{2011ApJ...727...20K}. Additionally, H$_2$O disk-masers like in UGC~3789 allow a direct measurement of angular diameter distance and the Hubble constant \citep{2013ApJ...767..154R}.

To date, over 4030 galaxies have been searched for H$_2$O masers, resulting in about 150 detections that include about 20 disk-maser galaxies (see e.g., \citealt{1995PASJ...47..771N, 1997ApJS..110..321B, 2005ApSS.295..107H, 2006ApJ...652..136K, 2008ApJ...678...96B, 2009ApJ...695..276B}; and the project web sites Water Maser Cosmology Project (WMCP)\footnote{\url{https://www.cfa.harvard.edu/~lincoln/demo/HoME/}} and Megamaser Cosmology Project (MCP)\footnote{\url{https://safe.nrao.edu/wiki/bin/view/Main/MegamaserCosmologyProject}}. In comparison, about 500 galaxies have been searched for OH masers, 120 were detected (at up to z\,$=$\,0.265), and about 10 exhibit OH in absorption (see e.g. \citealt{klockner,impellizzeri08}).

Sources that mase in both molecules are extremely rare. This may be expected, since extragalactic OH and H$_2$O maser species have a quite different pumping mechanism. While OH is radiatively pumped in regions of enhanced density by AGN or star formation photons reprocessed via $\ge45\,$K dust to 35/53\,\textmu{m} infrared (IR), gas phase H$_2$O is collisionally pumped at $\ge400$\,K.

Nevertheless, five objects that mase in both species are known: OH and H$_2$O kilomasers (OH~KM, H$_2$O~KM; ${L_\mathrm{OH}, L_\mathrm{H_2O}<10\,L_\sun}$) coexist in the starbursts NGC~253 \citep{1998AJ....115..559F,2004AA...414..117H} and M~82 \citep{1996AA...316..188B,2007MNRAS.380..596A}, an OH~KM and an H$_2$O megamaser (OH~MM, H$_2$O~MM; $L_\mathrm{OH}$, $L_\mathrm{H_2O}>10\,L_\sun$) are found in the Sy~2 NGC~1068 \citep{1996ApJ...462..740G} and radio-quiet Sy~2 AGN NGC~3079 \citep{1995ApJ...446..602B}, whereas Arp~299 is the only OH~MM and H$_2$O~MM object \citep{2007NewAR..51...67T}. No source with an OH~MM and an H$_2$O~KM has yet been found, likely because H$_2$O~KM tend to occur in nearby objects, whereas OH~MM are found up to high redshifts where H$_2$O~KM emission falls below sensitivity limits (see \citealt{2011AA...525A..91T}).

There is no clear general link between OH and H$_2$O maser species in such "dual-species" objects. However, OH maser emission (and OH seen in absorption) may point towards sources that contain denser molecular regions and a generally larger reservoir of H$_2$O; OH is formed from the evaporation and dissociation of grain-bound H$_2$O \citep{annurev.astro.41.011802.094927,2009ApJ...690.1497H}. A larger H$_2$O abundance may favor a H$_2$O maser detection. Furthermore, both H$_2$O~KM, OH~KM and OH~MM have a similar association with, amongst others, star forming regions and nuclear regions with bursts of intense star formation \citep{annurev.astro.41.011802.094927}. We consider that in a H$_2$O maser search, earlier OH detections could be one of the selection criteria that might increase the detection rate.

The search presented here attempts to identify new water maser galaxies, new dual maser species objects and in particular any H$_2$O~KM in an OH~MM galaxy, as well as new AGN disk-maser galaxies suitable for constraining the Hubble constant.

\section{Source sample}

We considered only sources within 250\,Mpc ($<$\,16\,000\,km\,s$^{-1}$). We first assembled a database of initially over 8000 known water maser detections and non-detections published in the literature, including WMCP and MCP project web site catalogs of published and unpublished maser search results. We then used an automated NASA/IPAC Extragalactic Database (NED) lookup of source coordinates and name aliases to merge duplicates. This produced a final catalog of 4038 unique objects already observed for H$_2$O.

Next we identified 126 galaxies in the catalog with a low sensitivity H$_2$O non-detection (40\,mJy to 200\,mJy rms) that could be reobserved with a factor 10 higher sensitivity. To identify new sources not yet observed at 22\,GHz, we reviewed recent X-ray and AGN data and literature, including recent extragalactic hydroxyl searches (e.g. \citealt{klockner,impellizzeri08}). We chose objects with {2--10\,keV} X-ray data, high X-ray luminosities (${L_\mathrm{X}  > 10^{40}}$\,W) and large absorbing column densities (${N_\mathrm{H} \gtrsim 10^{22}}$\,cm$^{-2}$) as found in over 90\,\% of water maser galaxies (e.g. \citealt{2006ApJ...652..136K,2006AA...450..933Z,2008ApJ...686L..13G}), and that have a nucleus classified as NLS1, Sy~1.5 to Sy~2.0, LINER or HII region. Some of the sources are also Infrared Astronomical Satellite (IRAS) survey objects with OH masers or OH seen in absorption.

The final selection of 40 nearby galaxies, mergers, binary AGN and triple AGN systems is shown in Table~\ref{tab:detectionlist} and consists of 17 previous non-detections at $\ge 40$\,mJy rms, 10 objects with OH seen in emission at 1.6\,GHz (3 being previous H$_2$O non-detections), 1 source with strong OH absorption at 6\,GHz (a previous H$_2$O non-detection), and 16 other sources not yet observed for 22\,GHz water masers. Out of this sample, OH maser galaxy ESO~320-G030 had the highest IRAS 100\,\textmu{m} flux density (46\,Jy).

\section{Observations}

To uncover kilomasers among the source sample a 4\,mJy rms target sensitivity over 24.4 kHz (about 0.31\,km\,s$^{-1}$) was chosen, equivalent to between $0.1\,L_\sun$~rms and $1.0\,L_\sun$~rms in isotropic luminosity. Observations were carried out in four runs during February and March 2013 under project AGBT13A-172 using the National Radio Astronomy Observatory (NRAO\footnote{The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.}) Robert C. Byrd Green Bank Telescope (GBT). Sessions were scheduled in late winter under good 22\,GHz weather conditions. UTC date and time and zenith opacity $\tau_0$ are listed in Table~\ref{tab:obsdates}. Excellent weather conditions (zenith ${\tau_{0}=0.033}$~to~$0.047$) and low $T_\mathrm{sys}$ (35~K to 75~K) allowed most of the 40 sources to be observed in 16 hours, spending between 12 and 20 minutes on each source and the remainder on calibration.

We used the GBT Spectrometer backend and GBT K-band Focal Plane Array (KFPA) receiver, and selected two KFPA elements near the cryo cooler with the lowest T\subscript{rx} ($<$25~K over 75\,\% of the band). Beams were 33$''$~FWHM with an aperture efficiency $\eta_{ap}$ of 0.66 at 21\,GHz and had a 94.9$''$ beam separation. Observations were in dual-circular polarization and had a 30 second dual-beam "nod" cycle. Both 200~MHz frequency windows of each polarization (i.e. 4 windows in total) were centered on the systemic velocity. The 8192 spectrometer channels were 24.4~kHz wide and covered $V_\mathrm{sys}\pm1250$\,km\,s$^{-1}$.

Pointing and focusing was corrected using strong standard calibrators ($>0.8$\,Jy). GBT dynamic corrections compensated for gravitational and thermal surface deformations and remained stable. The full setup was occasionally verified using brief pointings at megamaser galaxies NGC~1068, NGC~3079 and NGC~5793. Pointing and focusing were repeated every 1.5 to 2 hours and after sunrise, with only small adjustments ($<2.5''$ and $<8$\,mm). Wind speeds were low with little to no cloud cover. Zenith opacity measurements $\tau_0$ at 21\,GHz were supplied by nearby weather stations and remained stable during the observing runs.

\begin{table}
\caption{Observation dates.}\label{tab:obsdates}
\centering
\begin{tabular}{ccccc}
	\hline \hline
	Epoch & Start time (UT)  & Hours & $\tau_0$ \\
	\hline
	 1 & 2013-02-21 20:30 & 3:15 & 0.036--0.037 \\
	 2 & 2013-03-02 03:45 & 3:45 & 0.047 \\
	 ~ & 2013-03-02 07:30 & 1:30 & 0.043 \\
	 ~ & 2013-03-02 09:00 & 1:30 & 0.041 \\
	 3 & 2013-03-03 18:30 & 2:15 & 0.036 \\
	 ~ & 2013-03-03 20:45 & 1:15 & 0.033 \\
	 4 & 2013-03-09 11:15 & 2:15 & 0.036--0.035 \\
	\hline
\end{tabular}
\tablefoot{Start time, duration in hours and $\tau_0$ zenith opacity at 21 GHz of the four K-band observing runs
in project GBT13A-172.}
\end{table}

\section{Data reduction}

A conservative estimated of the flux scale accuracy is $\le 15$\,\%. All sources were observed in total power mode with $T_\mathrm{cal}$ noise injection to determine $T_\mathrm{sys}$. Although $T_\mathrm{cal}$ has a nominal accuracy of 1\,\%, slow temporal drifts degrade it to 10\,\% -- 15\,\% typical. The initial aperture efficiency $\eta_{ap0}$ calculated by the GBTIDL toolbox was corrected for elevation via the GBT 22.236\,GHz gain-elevation curve\footnote{\url{https://safe.nrao.edu/wiki/bin/view/GB/Observing/GainPerformance}} of April 8, 2008 that is based on the current Zernike model (\textit{FEM~plus~2005WinterV2}) for the GBT adaptive surface. The correction curve is ${\eta_{ap} = \eta_{ap0} * (0.910 + 0.00434*ZD - \num{5.22e-5} *ZD*ZD)}$ where $ZD = 90^\circ\, - \,\mathrm{elevation}$ is the angle off zenith.

Nod scans were processed in GBTIDL. The $\tau_{0}$ and $\eta_{ap}$ gain corrections were applied first. Next, subspectra affected by internal RFI or spectrometer faults were flagged. To improve the SNR, the blank sky reference subspectra (for subtracting the standing wave accross the band) were smoothed with a short 4 to 32 channel boxcar function. Care was taken to avoid introducing artifacts. Third order baselines were removed from individual subspectra. All subspectra and both polarizations were time averaged into a Stokes~I spectrum and a final 3\textsuperscript{rd}-order baseline fit was removed. Sensitivity was calculated over line-free channels without smoothing.

For each detection, Gaussian models ${S(\nu) = a*e^{-(\nu-\mu)^{2} / {2\sigma_{\nu}^{2}}}}$ were fitted into the calibrated non-smoothed spectra to estimate line peak $a$~(Jy), center $\mu$~(km\,s$^{-1}$) and FWHM width $w$~(km\,s$^{-1}$). The integrated line profile ${S_\mathrm{int}=\int_{-\infty}^{+\infty} S(\nu)\,d\nu}$ (Jy\,km\,s$^{-1}$) for a single Gaussian $S(\nu)$ equals ${a\,\sigma_{\nu}\sqrt{2\pi}}$. Further noting that ${\sigma_{\nu}=w/2.35482}$, and using the luminosity distance $D_\textrm{L}$ and redshift $z$ of the source, the equivalent isotropic luminosity of
\begin{equation}\label{eq:isolumdef}
\frac{L_\mathrm{iso}}{L_{\sun}}  = 0.023 \times \frac{S_\mathrm{int}}{[\textrm{Jy\,km\,s}^{-1}]} \times \frac{1}{1+z} \times \left( \frac{D_\mathrm{L}}{[\textrm{Mpc}]} \right)^{2}
\end{equation}
can be written for the fitted Gaussians in form of the sum
\begin{equation}\label{eq:isolumgauss}
\frac{L_\mathrm{iso}}{L_{\sun}}  = \frac{0.023 \sqrt{2\pi}}{2.35482} \times \frac{\sum\nolimits_{i} a_{i} \cdot w_{i}}{[\textrm{Jy\,km\,s}^{-1}]} \times \frac{1}{1+z} \times \left( \frac{D_\mathrm{L}}{[\textrm{Mpc}]} \right)^{2}
\end{equation}
over all Gaussian components (see also \citealt{2009ApJ...695..276B}). The factor 0.023 contains unit conversions and the water maser rest frequency (for 1.6\,GHz OH masers the factor is 0.0017). Upper luminosity limits for water maser non-detections are given for single wide Gaussian H$_2$O line with 2.0\,km\,s$^{-1}$ FWHM and a $3\sigma$ peak. The luminosities for detections are based on Eq.~\ref{eq:isolumdef}, with $S_\mathrm{int}$ evaluated directly over the line regions of the spectrum using Simpson's Rule. Spectra of the detections presented here were smoothed with a 3\textsuperscript{rd} order 9-point (2.79\,km\,s$^{-1}$) Savitzky-Golay shape-preserving filter to reduce the noise floor by 70\,\% while maintaining the shape and height of the maser features.

\section{Results and Discussion}

Of the 40 sources listed in Table~\ref{tab:detectionlist}, 37 were observed for H$_2$O masers with a detection rate of 11\,\%. Three sources have a strong maser detection and one has a tentative detection. The spectra are shown in Figure~\ref{fig:allspec}. Interestingly, three detections are in the set of 11 sources that are also detected in hydroxyl in emission or in deep absorption. No spectra were captured for three sources (NGC~3341, NGC~7130 and ESO~323-G077). The observed sources, sensitivities and isotropic luminosities (H$_2$O and OH), and absorbing column densities are given in Table~\ref{tab:detectionlist}. The luminosity distances, source redshifts and recession velocities, $v_{LSR}$, were adopted from NED. Recession velocities use the optical definition and are in the kinematic Local Standard of Rest (LSR).

Selection by X-ray data did not appear to enhance the H$_2$O maser detection rate. In our sample, 14 active galaxies have a published X-ray absorbing column density. Two of these yielded a H$_2$O~MM detection. One source hosts a heavily obscured AGN ($N_\mathrm{H} > 10^{23}$\,cm$^{-2}$) and the other a Compton-thick AGN ($N_\mathrm{H} \geq 10^{24}$\,cm$^{-2}$). This is consistent with \citet{2013arXiv1309.6515C} who find 96\,\% (45/47) of H$_2$O~MM sources have $N_\mathrm{H} > 10^{23}$\,cm$^{-2}$. However, the same two sources were also selected by OH, resulting in a better detection rate given by the OH selection (3/11) rather than the X-ray selection (2/14).

Below we discuss the four water maser detections.

\subsection{2MFGC~13581}

A new H$_2$O disk-MM is found in the optically edge-on galaxy 2MFGC~13581 (${v_\textrm{LSR}=10309\pm42}$\,km\,s$^{-1}$ \citep{2000AAS..142..417H}, ${D_\textrm{L}=145}$\,Mpc, ${z=0.034}$). It is the second-closest of six Seyfert candidates in the Hamburg/SAO survey for emission-line galaxies and is a probable Sy~2 \citep{2000AAS..142..417H}. Masers are detected in two high-velocity groups, symmetrically offset from the systemic velocity by about $\pm$390\,km\,s$^{-1}$. No systemic emission is detected and has a $3\sigma$ upper limit of 6.3\,mJy. The red group peaks at 25\,mJy and forms a forest of $\approx$3\,km\,s$^{-1}$ FWHM lines, similar to the blue group that peaks at 20\,mJy. Each group can be approximated by a wide profile, with the blue one centered at 9940\,km\,s$^{-1}$ (5.3\,mJy peak, 61.5\,km\,s$^{-1}$ FWHM) and the red one at 10724\,km\,s$^{-1}$ (4.4\,mJy peak, 114.4\,km\,s$^{-1}$ FWHM). Their mean, 10332\,km\,s$^{-1}$, lies within $1\sigma$ of the systemic recession velocity. The blue and red groups have luminosities of $120\,L_{\sun}$ and $170\,L_{\sun}$, respectively.

The symmetric spectrum suggests that emission most likely originates from a circumnuclear masing disk. The absence of systemic emission may be explained by a warp in the disk that shadows parts of the disk from the X-ray emission by the central engine that is thought to support maser emission \citep{1994ApJ...436L.127N}. The undetected systemic masers may also have a quite low flux density. Alternatively, they may be highly variable like the systemic (disk-)maser emission in Circinus and thus not always detected \citep{2003ApJ...590..162G,2009MNRAS.392.1339M}.

We can estimate the radius of the masing disk annulus in 2MFGC~1358 if we assume Keplerian rotation, a black hole mass of $10^7\,M_{\sun}$ typical of other disk-maser galaxies (e.g. \citealt{2011ApJ...727...20K}), and a fully edge-on disk. The observed orbital velocity of $\pm$390\,km\,s$^{-1}$ then translates into a 0.4\,parsec (0.8\,mas) average disk diameter. Unfortunately, given the low maser flux, prospects for a successful VLBI map and a determination of variability and the secular acceleration of possibly existing weak systemic maser components are poor.

\subsection{IRAS~17526+3253}

Water megamasers in this IR galaxy ({UGC~11035}; ${v_\textrm{LSR}=7818\pm9}$\,km\,s$^{-1}$ \citep{1991rc3..book.....D}, ${D_\textrm{L}=108}$\,Mpc, ${z=0.026}$ (NED), ${L_{IR} \approx \num{7e11} L_{\sun}}$ estimated from IRAS fluxes using the method by \citealt{1986AA...168..237W}) have a relatively high peak flux of ${\approx{170}}$\,mJy. Emission appears in a narrow, slightly blueshifted 40\,km\,s$^{-1}$ window around the systemic velocity. It has three features: two wider profiles at 7797\,km\,s$^{-1}$ (47\,mJy peak, 4.0\,km\,s$^{-1}$ FWHM, $50\,L_{\sun}$) and 7810\,km\,s$^{-1}$ (65\,mJy peak, 10.9\,km\,s$^{-1}$ FWHM, $210\,L_{\sun}$), and a narrow emission line at 7808\,km\,s$^{-1}$ (170 mJy peak, 2.2\,km\,s$^{-1}$ FWHM, $100\,L_{\sun}$).

Literature lists UGC~11035 as an OH~KM galaxy. An early non-detection (${L_{OH} < 4\,L_\sun}$ at 1.0\,mJy~rms) by \citet{garwood87} was followed by a broad blueshifted feature (3.7\,mJy peak, ${L_{OH} = 6.46\,L_\sun}$) detected near 7450\,km\,s$^{-1}$ by \citealt{1989CRASM.308..287M} but no spectrum was published. A recent observation suffered from RFI and had insufficient sensitivity to confirm the kilomaser \citep{2013ApJ...763....8M}.

The 2MASS image shows two near-infrared components separated by 60$''$ (about 30\,kpc) with an angular size ratio of $\approx 5$. The image suggests UGC~11035 could be a major merger system. The hard X-ray luminosity would then be expected to exceed $10^{43}$\,erg\,s$^{-1}$. This would contribute to enhanced IR luminosity through core emission reprocessed in the dense concentration of gas accumulated during the merger event. Using 60\,\textmu{m}, 100\,\textmu{m}m and S$_{1.4\,\mathrm{GHz}}$ flux points from NED, the $q$ parameter (see e.g. \citealt{2001ApJ...554..803Y}) of this galaxy is 4.74, indicating an IR excess. The $q$ is notably higher than 2.34$\pm$0.01 of the IRAS 2\,Jy sample \citep{2001ApJ...554..803Y} and exceeds 2.57$\pm$0.36 of typical OH~MM galaxies \citep{klockner}, indicating a buried AGN or enhanced star formation. UGC~11035 also has a curiously flat velocity field of 210\,km\,s$^{-1}$ at 9\,kpc from the center, suggesting either a giant irregular galaxy or interaction of two face-on objects. The inner 18\,kpc have a kinematic mass of ${\approx 10^{11}\,M_{\sun}}$ \citep{1992AIPC..254..617A,1994AAS..107...23A}.

Given limited data on the object we speculate that H$_2$O emission might originate from a small shocked region in an ongoing merger similar to Arp~299. The maser features lack the high velocities associated with jet and nuclear outflow masers (e.g. \citealt{2003ApJ...590..162G}). Their velocity span of 40\,km\,s$^{-1}$ is narrow, but still typical of star formation masers. Assuming a buried AGN gives rise to the IR excess, the systemic masers may also be associated with a slightly inclined, not fully edge-on warped accretion disk. A warp along the line of sight towards the nucleus can compensate for the disk inclination and produce the velocity coherent path lengths necessary for luminous systemic maser emission. Monitoring for secular line accelerations or a VLBI observation are required to rule out a nuclear association.

\subsection{NGC~4261}

The WMCP project lists the giant elliptical galaxy NGC~4261 (${v_\textrm{LSR}=2240\pm7}$\,km\,s$^{-1}$ \citep{2000AJ....119.1645T}, ${D_\textrm{L} = 35.6}$\,Mpc, ${z = 0.0075}$) as a 109\,mJy~rms non-detection observed in 2002. We reached 3.1\,mJy~rms and detect broad emission that is fitted by a single Gaussian of 10.3\,mJy, 154\,km\,s$^{-1}$ FWHM centered on 2302\,km\,s$^{-1}$. Peak emission is redshifted by about +60\,km\,s$^{-1}$ relative to the systemic velocity and has a total isotropic luminosity of $50\,L_{\sun}$.

NGC~4261 is a LINER galaxy associated with the low-luminosity FR-\Romannum{1}{} radio source {3C\nobreak\,270} that launches a highly symmetric kpc-scale twin jet. The galaxy is known for its 240\,pc nuclear torus/disk found by the Hubble Space Telescope. The nucleus hosts a \num{4.9e8}\,$M_\sun$ SMBH and has an X-ray absorbing column density $N_\textrm{H}$ of $>\num{5e22}$\,cm$^{-2}$ \citep{2003AA...408..949G}. Recent hard X-ray data show a slightly higher obscuring column density of ${16.4^{21.64}_{13.25} \times 10^{22}}$\,cm$^{-2}$ \citep{gonz09}.

VLBI shows neutral H\,\Romannum{1}{} absorption against the counter-jet, with deepest absorption at 2260\,km\,s$^{-1}$, redwards with respect to the systemic velocity. It has been modeled by atomic gas in a thin disk with an absorbing column density of ${N_\mathrm{H} \approx 10^{21}}$\,cm$^{-2}$ \citep{2000AA...354L..45V}. There is also deep OH absorption at 6\,GHz against a 1.3\,Jy continuum with a $400$\,km\,s$^{-1}$ FWHM around the systemic velocity \citep{impellizzeri08}.

With the presence of a low-luminosity core, an optical dusty torus, molecular absorption and a twin radio jet, NGC~4261 is remarkably similar to the twin-jet LINER NGC~1052. The spectrum of NGC~1052 has a single, broad and slightly redshifted luminous 150\,mJy maser feature. VLBI observations of NGC~1052 found water masers in two regions along the jet axis. Emission has been associated with continuum seed emission from jet blobs being amplified in a X-ray dissociation region located on the inner surface of a torus at a typical (for a J-type shock) temperature of 400\,K \citep{2008ApJ...680..191S}. Given the evidence for abundant H\,\Romannum{1}{} and OH molecules and a high X-ray absorbing $N_\mathrm{H}$ column density towards NGC~4261, combined with the radio jet and the maser profile, a masing torus region with gas infalling at +60\,km\,s$^{-1}$ seems plausible. Existing VLBI datasets map only NGC~4261 continuum emission and do not cover the maser frequency range. A VLBI follow-up is required to determine a masing torus association.

\subsection{IRAS~20550+1656}

We tentatively find broad megamasers in the LIRG/ULIRG irregular galaxy IRAS~20550+1656 (II~Zw~96; ${v_\textrm{LSR}=10837\pm10}$\,km\,s$^{-1}$ \citep{1993AJ....105.1271G}, ${D_\textrm{L}=148}$\,Mpc, ${z=0.036}$). With Arp~299, IRAS~20550+1656 may be the second galaxy that hosts megamasers of both the OH and H$_2$O species. The sensitivity was 5.8\,mJy per 0.3\,km\,s$^{-1}$ channel and 1.5\,mJy after 16-channel Gaussian smoothing. Two 9\,mJy features are seen at $\pm110$\,km\,s$^{-1}$ around the recessional velocity. The combined isotropic luminosity of the blue 10737\,km\,s$^{-1}$ feature (9.0\,mJy peak, 102.8\,km\,s$^{-1}$ FWHM) and the red 10957\,km\,s$^{-1}$ feature (9.1\,mJy peak, 96.4\,km\,s$^{-1}$ FWHM) is relatively high with $600\,L_{\sun}$. Narrower features seem to be symmetrically distributed around the systemic velocity, such as two offset by $-380$\,km\,s$^{-1}$ and $+420$\,km\,s$^{-1}$, but could also be explained as particularly pronounced baseline ripple. These and the broad features are however persistent over different smoothing settings for the "nod" reference spectra, and different baseline fits prior to averaging all subspectra. The broad masers have a post-fit confidence of somewhat better than $5\sigma$. The GBT integration time was 12 minutes and additional time would be needed for a more robust detection especially of the narrower features.

The object is an ongoing merger or close binary system with a peculiar rotation curve that is known to host an OH~MM with 26\,mJy peak and $83.2\,L_{\sun}$ luminosity \citep{1992AIPC..254..617A,klockner}. H\,\Romannum{1}{} is seen in emission with a FWHM of about $200$\,km\,s$^{-1}$ \citep{2001AA...368...64V}. XMM-Newton observations found a single X-ray source and a high abundance of alpha process elements suggestive of starburst activity, but could not rule out an AGN or AGN-starburst composite. The X-ray core is either very faint or has an ${N_\mathrm{H} > 10^{24}}$\,cm$^{-2}$ \citep{2010AJ....140...63I,2012arXiv1211.1674M}. Starburst activity would be consistent with earlier optical and IR spectroscopy \citep{1997AJ....113.1569G}. VLBI observations of the OH~MM emission have placed it off-center in a merging system. The OH masers trace a 300\,pc region around the second nucleus with a mass of $10^9\,M_{\sun}$ that has some probability of being a heavily obscured AGN \citep{2011MNRAS.416.1267M}. Spitzer observations found starburst activity similar to extranuclear starbursts in NGC~4038/9 and Arp~299. In the latter, three maser regions are associated with both nuclear regions of Arp~299 and an overlap region \citep{2011AA...525A..91T}. The spectrum of the IRAS~20550+1656 water masers is also strongly reminiscent of that of NGC~2146 with its massive star formation kilomasers. The data are quite suggestive that IRAS~20550+1656 masers can be related to starburst and star formation activity. The maser flux is unfortunately rather low for a VLBI follow-up.

\section{Dual maser species}

In literature, there are five known sources (or six, if including uncertain OH masers in UGC~5101) that are known to host both OH and H$_2$O maser species. These "dual-species" objects typically have a complex morphology and the masers are located in unrelated regions. Our two detections in 10 searched OH maser objects increase the number of known dual-species objects to eight.

\citet{2011AA...525A..91T} report 57 sources searched for both 1.6\,GHz OH and 22\,GHz H$_2$O maser species. Six are detected in neither species, 45 in only one, and six in both species. Tarchi et al. also note a curious lack of H$_2$O~kilomasers in OH~megamaser objects. Adding our sources, and sources common to the 4038-entry H$_2$O database and recent OH searches \citep{1992MNRAS.258..725S,klockner,impellizzeri08,0004-637X-730-1-56}, we find a total of 95 sources searched for both transitions, 34 detected in neither, 35 detected in H$_2$O only, 18 in OH only, and about 8 detected in both species (if the two uncertain OH masers in UGC~5101 and IRAS~17526+3253 are included), for a total of 61 sources detected in at least one of the two maser species. Luminosities, $3\sigma$ limits and redshifts of these 61 detected sources are presented in Figure~\ref{fig:OHxH2O}. Luminosities against source redshifts for all 95 sources are shown in the inset. The upper limits of the non-detections have a median of 0.04~$L_\sun$ for OH and 0.4~$L_\sun$ for H$_2$O. This demonstrates a large fraction of H$_2$O kilomasers ($L<10\,L_{\sun}$) may go undetected. The difference in the two medians is partly due to the frequency proportionality of the isotropic luminosity in Eq.~\ref{eq:isolumdef} -- an at least factor 13 higher sensitivity (lower mJy~rms) is required for detecting H$_2$O~kilomasers at 22\,GHz in a 1.6\,GHz OH~MM object. The probability of detecting a H$_2$O~KM in OH~MM objects is further reduced by the higher average redshift of OH~MM galaxies, with currently known H$_2$O~KM galaxies found at redshifts up to $0.014$ and OH~MM galaxies at redshifts between $0.010$ and $0.264$.

The six reliable dual-species detections correspond to a conditional water maser detection rate of ${P(\mathrm{H_2O}|\mathrm{OH})}=25\,\%$ in the 24 OH~galaxies, and a detection rate of ${P(\mathrm{OH} \cap \mathrm{H_2O}|s_1)=6\,\%}$ for all $N=95$ targets selected for an OH search by some criteria $s_1$ such as high infrared flux density. Over current searches, the average detection rate for OH is about ${P(\mathrm{OH}|s_1)=25\,\%}$ (120 in 500) and about ${P(\mathrm{H_2O}|s_2)=4\,\%}$ for H$_2$O (150 in 4030), where the selection criteria $s_2$ typically include starburst or AGN activity, X-ray luminosity or a high absorbing column density $N_\mathrm{H}$. Accounting for apparently mutually exclusive pumping mechanisms of the OH and H$_2$O species and assuming selections $s_1$ and $s_2$ are independent (although \citealt{2004ASPC..320..199T} find a significantly increased H$_2$O maser detection rate in FIR-luminous sources), the lower bound for the expected probability of two species independently coinciding would be ${P(\mathrm{OH} \cap \mathrm{H_2O}|s_1,s_2) \ge 1\,\%}$, which is on the order of 6\,\% of the $N=95$ dataset. An accurate estimate of the coincidence rate would require a comparison of the selection criteria of each of the 95 sources, a task that is beyond the current scope.

\section{Conclusions and Summary}

We detected water megamasers in four galaxies: three in OH galaxies, and one in a Sy~2 galaxy with no previous OH search. The OH~MM galaxy IRAS~20550+1656 has a tentative starburst-like H$_2$O~MM detection, the presumed OH~KM galaxy IRAS~17526+3253 has narrow 0.17\,Jy systemic masers, and the 6\,GHz OH absorber NGC~4261 (3C~270) with a twin jet hosts a likely jet-maser. Disk-masers were found towards the probable Sy~2 AGN in 2MFGC~13581. The black hole mass is unknown, but assuming a mass of $10^7\,M_{\sun}$ typical of AGN disk-maser galaxies, the masing disk may be around 0.4\,pc in diameter. Masers in NGC~4261 are particularly interesting as the host galaxy and the maser profile are remarkably similar to H$_2$O~MM galaxy NGC~1052. A VLBI map of NGC~4261 may be able to locate regions of a molecular torus excited by a background jet continuum like in NGC~1052. VLBI imaging of disk-maser galaxy 2MFGC~13581 might produce a precise $M_\mathrm{BH}$ estimate, although the maser flux densities are very low for VLBI. Lack of systemic features in 2MFGC~13581 makes this source less interesting for measuring the angular diameter distance and the Hubble constant. We plan VLBI follow-ups on the more luminous detections in IRAS~17526+3253 and NGC~4261.

Our detection of water masers in two OH maser galaxies updates the current count of six dual-species objects to eight. The conditional H$_2$O detection rate in OH maser galaxies $P(\mathrm{H_2O}|\mathrm{OH})=25\,\%$ is higher than the average 4\,\% rate achieved in H$_2$O maser searches. We could speculate that OH masers point towards systems with an overall larger molecular reservoir or a larger number of over-densities and shocked regions with favorable conditions for producing detectable luminous H$_2$O maser emission. The dual-species detections in a sample of 95 objects may be explained by a random coincidence of two regions with suitable maser conditions in a single system. However, a more detailed analysis that inspects actual source selection criteria of each of the 95 sources is necessary to determine if dual-species detections are indeed a random coincidence, and if the seemingly enhanced detection rate of H$_2$O masers in extragalactic objects selected by the presence of OH masers is only a product of the small dataset.

\begin{acknowledgements}
I thank Jim Braatz, Christian Henkel, and Alan Roy for introduction to the GBT, discussion during the proposal, and comments on the manuscript. The author was supported for this research through the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


text:
UK Section
AES UK Section Committee
AES UK Section Volunteers
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Latest AES Events
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Up Your Output!
15th UK Conference 1999
This invaluable conference provided a comprehensive update of the current themes in audio engineering, and the future trends which will affect the audio industry as a whole.Read more
Audio - The Second Century
Audio has traditionally been seen as a self-contained discipline, but increasingly it is being combined with other technologies to create systems which are, in the broadest sense, multi-media. The constraints under which we work are evolving, and the technology with which we work is advancing relentlessly. Standards can no longer treat audio in isolation, and are becoming centred on applications, rather than technologies.
The availability of multi-channel home-delivery formats, the increasing importance of both live and cinema sound, and the abundance of cheap computing power are all having fundamental influences across the industry, from recording studio to sitting room. Audio quality is threatened by increasing demands for data compression and the consumers' expectations for tumbling prices in the High Street. This is particularly prevalent in areas such as PC sound and home cinema which are perhaps seen as being on the fringes of the traditional audio industry.
The goalposts have moved.
The conference covered the technologies and techniques which we can apply to this new range of problems. A guide to the effective handling of multi-channel and low bit-rate audio was combined with coverage of the latest DSP and computer technology and standards. This showed how high engineering standards could be applied in areas where audio has too often been relegated to second place. It will gave an insight into how audio engineering can adapt to new applications and enable us to compete effectively in new market areas.
Click here for the detailed conference programme.
Click here for the detailed conference report.
Archive link
← 26th UK AES Conference on Audio Education
16th UK Conference 2000 →
26th UK AES Conference on Audio Education University of Glasgow, Scotland 26th – 28th August 2015
info@aes-uk.org
Copyright © 2020 Audio Engineering Society

redpajama_set_name: RedPajamaCommonCrawl


The sea and the moon, the pine trees and a modern Greek version of the traditional, simplistic way fish is prepared and served.
Celebrity visitors like Bill Clinton, Sean Connery, and Julio Iglesias have left their mark here. It's pricey, but if Connery paid the bill with a smile, so will you.


text:
The 2001 California Golden Bears football team was an American football team that represented the University of California, Berkeley in the Pacific-10 Conference (Pac-10) during the 2001 NCAA Division I-A football season. In their fifth and final year under head coach Tom Holmoe, the Golden Bears compiled a 1–10 record (0–8 against Pac-10 opponents), finished in last place in the Pac-10, and were outscored by their opponents by a combined score of 431 to 201.

The team's statistical leaders included Kyle Boller with 1,741 passing yards, Terrell Williams with 688 rushing yards, and Charon Arnold with 606 receiving yards.

Following a loss to Arizona and an 0–8 start, Holmoe announced his resignation effective at the end of the season.

Schedule

References

California
California Golden Bears football seasons
California Golden Bears football

redpajama_set_name: RedPajamaWikipedia


text:
Q: How can I move a discussion to chat before being prompted? I posted an answer to a question, and a user posted a comment that I feel is better handled in chat.  In a previous question, I was prompted to move the comment to chat when it went over a certain limit.  Can I move comments to chat without having hit that limit?

A: There are a few options to move comments to chat. You can create your own chat room and manually invite the other user to chat. You can also add a few extra messages to the conversation in the comments so that the option to move the conversation to chat comes up. You can then delete the extra messages and possibly tell the other user what you were doing. One last option is very cool, but can only be done by a moderator on the site where the conversation is taking place. All that you have to do is this command into the Javascript console:
$.post('admin/posts/' + post_id + '/move-comments-to-chat', {fkey:StackExchange.options.user.fkey});

where post_id is the id of the post with the comments you want to move to chat (obviously). This will leave a comment inviting the other user to chat, but the messages will still have to be manually deleted, which is easy if you are a moderator.

This is a bot run by @michaelpri a moderator on two SE sites

A: agf's comment is correct.  Move the discussion to chat by discussing in chat, and stop commenting on the post.  If the other user doesn't want to move, that's OK, you don't have to discuss it. Flag one of the comments for moderator cleanup if need be, and move on :)

redpajama_set_name: RedPajamaStackExchange


I own one and so far it is great car .
This car is really great! Especially for first time drivers! There's not a lot of blind spots and it's easy to maneuver. I would keep this car if my needs had not changed since buying!


text:
[0] => https://i0.wp.com/watermission.org/wp-content/uploads/2019/12/November-Campaign-Header.jpg?resize=1600%2C520&ssl=1
George Greene III, PE, PhD
Co-founder, Executive Chair
George Greene III, PE, PhD, is the co-founder and Executive Chair of Water Mission. In this role, he leads the strategic direction of Water Mission along with the board of directors, while also continuing to actively direct strategic key projects. Additionally, Dr. Greene serves as the Chair of the Board of Directors and Interim Executive Director of the Global Water Center, an independent 501(c)3 founded by Water Mission. The Global Water Center's mission is to end the global water crisis by developing collaboration among global organizations, incentivizing, and equipping them to work to internationally accepted standards.
Prior to co-founding Water Mission with his wife, Molly, in 2001, Dr. Greene founded General Engineering Laboratories (GEL), serving as CEO and chief engineer for 20 years. Dr. Greene led the company to become one of the largest privately-held environmental laboratories in the United States. In addition, Dr. Greene has worked as a chemical process design engineer at Lurgi in Frankfurt, Germany, and as the team leader of the Residuum Conversion Math Modelling Team at Exxon Research and Engineering.
Dr. Greene received his doctorate in chemical engineering from Tulane University, his master's degree in chemical engineering from Columbia University, and a bachelor's degree in chemical engineering from the University of Florida. He is a licensed professional engineer and holds several patents related to water treatment.
In 2008, Dr. Greene was awarded an honorary Doctor of Public Service from Charleston Southern University. He and his wife have also received The Order of the Palmetto, South Carolina's highest civilian award, and Rotary International's Service Above Self Award. Most recently, in 2022, Dr. Greene was inducted into the South Carolina Business Hall of Fame for his accomplishments as a business leader who continues to inspire others to take action joining the effort to end the global water crisis. Dr. Greene is an active member of St. Philip's Church, an Anglican church in Charleston, SC.
Back to Leadership


text:
ZISRE TECH
Contribute page
It all began when our CEO Zain Ahmed started working in the Retail & hospitality industry at a young age for businesses which were owned by family&friends. It was here Zain noticed that Staff can be very unreliable in the hospitality industry. He always thought the staff were to blame as he presumed they were taking advantage of the business owners. However, after looking into the roles he realised that these staff faced a lot of high pressure & stress. That's when he began thinking of ways to make their jobs easier. He realised that if the businesses made the jobs less stressful for the employees by using the right machinery then the employees would be under less stress & pressure. If business owners could find a way to lower the pressure & stress employees face, they would see a higher employee retention rate, that is when Zain began researching the robotics industry to see how robots can benefit businesses without taking over jobs.
However, as Zain was doing his research in the industry he noticed a lot of elderly people that live alone who need support, and don't have access to fresh meals. They always needed to constantly rely on support workers or family for fresh home-cooked meals, and when the support was not available they had relied on microwavable & takeout food, which in the long term can deteriorate their health.
So Zain decided that before going into the business sector he would make it his mission to give support to those who need it most
Redefining the Way
Our mission is to give support to those who need it most. We want our Robots to be cost-effective for every household worldwide and create a stress-free work environment for our everyday employees who are the face of our nation. The most important part of the engineering perspective is trying to ensure as much of our materials are recyclable & reusable for the future. If we are developing robots to help the people then we as a company believe we should do our best to respect the land we live on.
Our Journey So Far
It was in 2013 when Zain Ahmed realised that robots could help the masses.
The first steps
Between 2013-2018 Zain was focused on his career & never had the time to think about the robots, but around 6 months into 2018 Zain decided it was time to do something about it.
HELLO@ZISRETECH.COM
© 2022 by Ziser Tech.


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Microsoft opens its doors to game developers
by Builder Staff in After Hours on February 22, 2008, 3:06 AM PST
Microsoft has announced that it will soon make it possible for its Xbox LIVE members to develop and share their creations with the community online.
The new community-developed games are expected to double the size of the Xbox 360 game library, allowing the users to enjoy over a 1000 games by the end of 2008.
"The time has come for the games industry to open its doors to all game creators, enabling anyone to share their creations with the world," said John Schappert, corporate vice president of LIVE, software and services for the interactive entertainment business unit at Microsoft. "Our goal is to drive a creative and social revolution in games with the same transformative power that we've seen in digital music and video sharing."
The news comes after Microsoft announced its DreamSpark initiative this week, which makes software tools, including XNA Game Studio 2.0 for developing Xbox 360 games, available free to students free to students.
Chris Satchell, general manager and chief XNA architect at Microsoft, said seven games developed with XNA Game Studio 2.0 are now available, including JellyCar, LittleGamers, The Dishwasher: Dead Samurai, TriLinea, RocketBall, ProximityHD and Culture.
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Avem placerea sa va invitam la workshop-ul "Engineering Modelling & Simulation - Where We Are, Near Future Trends" care va avea loc joi, 12.05.2016, ora 15:00 la Facultatea de Inginerie, corp cladire G, sala G208.
conjunction with the modern High Performance Computing hardware. 2.	A brief presentation of the HPC system (52 processors, 624 cores) from "Dunarea de Jos" University of Galati.
•	Automotive applications - vehicle drag estimation and the assessment of forces and moments acting on the vehicle during crosswind driving using accurate Large Eddy Simulation modeling.


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Houston Weather in August
by Liz Osborn CurrentResults.com
August is the hottest month for Houston, Texas. That means most days have highs in the mid 90s degrees Fahrenheit (around 35 degrees Celsius). Thunderstorms are common now and so is sunshine.
This page gives detailed information on the typical August temperature, precipitation, sun, humidity, wind and storms for Houston. The numbers here are historical averages based on temperature and rainfall measurements gathered at Houston Hobby Airport and other climate data from George Bush Intercontinental Airport.
94 °F August average high 34 °C
77 °F August average low 25 °C
August is Houston's hottest month overall, with temperatures peaking from the 1st to 13th. These dates have daily highs averaging 94 °F (34 °C) and lows of 77 °F (25 °C).
26 days 90 °F max. or more (32 °C)
1 day 70 °F min. or less (21 °C)
Usually every day in August is at least 80 °F (27 °C) in Houston. The city averages one or two days this month when the thermometer reaches into the 100s °F (over 38 °C).
Normally August never cools down to 60 °F (16 °C) at night.
5.4 in total precipitation 138 mm
10 days of rain
Half the time, Houston receives 2.0 to 7.2 inches (51 to 183 mm) of rainfall in August. One in four years has drier weather, while another one in four is wetter.
68 % sunshine
6 days clear skies
The sun's rays reach the ground in Houston during 68 percent of daylight hours on average in August, for a total of 277 hours in the month. Typically on 6 days this month the sky is mainly clear, with at most 30 percent cloud cover.
Sunlight in August at Houston lasts for 13 hours and 10 minutes a day on average. The longest day of the month is the 1st with 13 hours and 33 minutes of daylight. By the end of the month, the days have shortened to 12:46 from sunrise to sunset. These durations can vary by a minute or two from year to year.
75 % August average humidity
The relative humidity in Houston during August usually peaks at 93 percent in the morning then drops to 55 percent by mid afternoon.
Local Time 12 am 3 am 6 am 9 am 12 pm 3 pm 6 pm 9 pm
Humidity % 88 92 93 74 58 55 63 79
6.1 mph August wind speed average 9.8 kph
August is the least windy month at Houston.
3 days rainfall of 0.5 inches (13 mm) or more
10 days with thunderstorms in August
14 % chance a named storm approaches
There's a 4 percent probability that a hurricane will approach within 100 miles (165 km) of Houston during August. The chance of a major hurricane (category 3 to 5) reaching the area is 1 percent.
The weather data here are long-term averages provided by the US National Centers for Environmental Information (NCEI). Temperature and precipitation are 1991-2020 normals while humidity and thunderstorms are 1961-1990 normals. The named storm probabilities come from the Atlantic Oceanographic and Meteorological Laboratory, Hurricane Research Division.
More Climate Information
Houston Weather in July
Houston Weather in September
Houston Temperatures: Averages by Month
Texas Weather Averages
USA > Texas >


Coin Collecting: How To Tone Coins Naturally And Increase Coin Value.
Research in detail about Antique Coins of India and Rare Coins of British.Coins can be fun to collect, but finding the value of a coin takes time. Your search for Julius Caesar matched 652 lots. Heritage World Coin Auctions - ANA.
Antique gold coins can make a good buy but there are a number of.Antique coins values - 484 results from brands Dayana U, Safavieh, Il Bisonte, products like Tech Lighting 700MORIVOB MonoRail River Rock Oval Blue Slate Hand-Blown.
We specialize in valuing and buying all type of antique advertising collectibles.
The value is based on the condition,. the collector term only refers to coin notes from 1890 or 1891,.
Colonial Coins were issued when India was colonised by the British, Portuguese, Dutch, etc.Antique coin values - 528 results from brands Dayana U, Safavieh, Il Bisonte, products like Dayana U Ohio State Buckeyes Silver Antique Coin Tie Bar, Tech Lighting.
About 97% of these are metal crafts, 47% are souvenirs, and 32% are folk crafts.
CanadaCurrency.com is the leading guide used by collectors and dealers to value and price old and rare. to value and sell their currency or get coin values.
Find out with our Quick Reference Guide to Paper Currency at Heritage Auctions. premium over face value.
For example, one edition will lists all recorded coins from 1901-2000.Coin collecting: Coin collecting. or alternatively possessing a substantial token value, coins have always been prized,. demand for antique coins greatly.
Rare and antique coins become new investment as their. coins become new investment as their prices surge. The rarity of any collectible item will drastically affect its value.Antique Silver: Coin Silver vs. Sterling. sterling silver can be found in some coins, the most famous example of which is the. its value is mainly determined.


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Stella Blakemore était une écrivaine sud-africaine auteur de romans pour enfants en afrikaans.

Biographie
Stella Blakemore est née dans une tente près de Lindley dans la Colonie de la rivière Orange le 13 avril 1906. Elle est allée à l'école au Natal. Sa mère, Emmarentia Susanna Catherina Krogh, était une professeure de musique d'origine boer et son père était le capitaine Percy Harold Jenks Blakemore, officier dans l'armée britannique. Le capitaine Blakemore a quitté sa femme et son enfant quatre ans plus tard pour devenir un joueur de cartes professionnel. Le pseudonyme le plus célèbre de Stella Blakemore, Theunis Krogh, est dérivé de son grand-père du côté maternel - Theunis Johannes Krogh, sous-secrétaire de l'administration sud-africaine du président Paul Kruger. En 1933, elle épouse le Gallois David Owen, ingénieur civil à Londres, ce qui fut le début d'une longue période de voyages dans le monde pour elle. Le couple a vécu, entre autres, au Ghana, en Côte d'Ivoire, en Italie, en Angleterre, au Swaziland, au Nigeria, en Allemagne et en Irlande. Le couple a eu deux enfants, Peter et Salene, tous deux adoptés. Stella Blakemore est décédée à Rostrevor, Newry et Mourne, en Irlande du Nord, au Royaume-Uni, à l'âge de 85 ans en mai 1991.

Œuvres
 Die Goue Sleutel ("The Golden Key"), 1920.
 Die Meisies van Maasdorp ("The Girls of Maasdorp"), 1932.
 Keurboslaan series (20 livres sous le pseudonyme de Theunis Krogh).
 66 livres au total sous les noms d'Analize Biermann, Stella Owen et Diem Grimbeeck.

Notes et références

Écrivain sud-africain
Naissance en avril 1906
Décès en mai 1991
Décès à 85 ans
Romancière sud-africaine


Located in the lap of the Himalayas of the rain shadow region, this divergent mountain desert enclave was only recently opened to westerners ( 1988 ) and therefore, requires a special permit to enter.
Fly into Juphal and proceed north to enter the Phoksundo National Park and tarace the steps of the famous writer of the book "The Snow Leopard", Peter Matthiessen. The trek passes over the Kang La Pass ( 5279 m / 17,320 ft ) and then the Crystal Mountain to reach the 7th century Shey Gompa ( Monastery ). On the way we pay a visit to one of the most secluded villages of Upper Dolpo. These are areas where locals still embrace the ancient pre-Buddhist Bon Po religion and villagers adorn themselves in Tibetan finery.
The remoteness of the Upper Dolpo region offers the hiker who prefers a more raw, yet culturally diverse experience.


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Q: MYSQL Database Structure for 2-round Events I'd like to create a database to store information about events with the following details for each record:
Event, Player 1 name, Player 2 name, Final score

Round 1:
Date, location, Important detail 1, Important detail 2

Round 2:
Date, location, Important detail 1, Important detail 2

Could someone tell me how this would translate to a mySQL database please? I mean by that a suitable database name, whether I need one or multiple tables, what fields I need to create.
I might be over-complicating things in my mind, but I'm wondering if there are "layers" in a database or whether I would just have individual fields such as round1 date, round1 location, ...., round2 date etc, as opposed to something like event1 rounds with sub tables for each round.

A: When naming database it is normally project or company name.
in this case your game name
for keeping data you need to consider normalization rules. from that you can think how many tables and which table data should go.
in this case one event has multiple rounds
when naming tables i prefer prefixing parent so things can be find easily.
So putting altogether
Database name: company/game name
event
event_id(unique),   player 1,   player 2,   final score ,
event_round
event_id,   round_id(unique),   round number,   date,   location,
event_round_important
round_id,   important_data,


After completing my pre-registration year at an Independent Opticians, I joined Specsavers Lichfield as a newly qualified optometrist. I had an 18 month hiatus with a well-known competitor and came crawling back! I then worked at Birmingham New Street's flag ship store before joining Specsavers Worcester as Ophthalmic Partner.
My first role within Specsavers at Lichfield enabled me to gain experience as a clinician, become accredited to perform Glaucoma refinement, as well gain an understanding of the 'Specsavers Way'. Whilst working for a competitor I gained management experience but soon realised it was not for me! Joining Birmingham New Street store, alongside completing the Pathway Development programme, gave me a great insight into all areas of the business, both clinically and commercially.
Specsavers have supported my development in every which way. Clinically, CET is readily available and PAC is always a success. Whilst working for Specsavers I have been able to complete further accreditations in Glaucoma refinement and MECS. Commercially, I progressed through the Pathway programme. I found this extremely eye opening and informative; a great platform to prepare you for starting life as a Partner.
Enhanced Optical Services are a great step forward for Optometry; a great utilisation of the clinical skills we have within our businesses. OCT is on the horizon and is an exciting proposition for Specsavers and the relationship with our medical partners in Ophthalmology departments across the nation.
We are heavily involved with community eye-care. We provide MECS, Glaucoma refinement, and post-cat appointments to our patients. We are about to embark on an agreed pathway whereby children with vision defects picked up at school screenings will be referred to us as opposed to secondary care. A great step forward for all involved.
Where do you think you have made a real difference to someone's eye health?
I remember testing a young girl who had been experiencing headaches for over 9 months, regular GP visits and treatment were not helping. Her mother bought her in for an eye examination and when checking the back of the eye I noticed swelling at the optic nerve. She was seen in hospital clinic the next morning, a brain tumour was diagnosed and was rushed over 100 miles to a specialist paediatric surgeon for it to be removed. The family came in the following week to thank me for saving her life. That was quite an emotional and rewarding day!
We are very passionate here in Worcester in this respect. We attend local events run by our LOC and by our local private hospital eye department. We all attend PAC and all eight optometrists who work here are accredited to perform Post-cat assessments, MECS and Glaucoma refinement. We are all looking forward to developing even further with OCT imminent. As a team, we embrace change and can see the positive impact it has on the local community.
From my very first interview at Specsavers Lichfield I knew I wanted to become an Ophthalmic Partner. I am proud that with the right support I have managed to achieve this. I am a personal example of why Specsavers is a great company to work for; if you work hard, Specsavers will support you in every way they can.


text:
Olivia Lutterman
Physics, Secondary Education
"The math faculty are super supportive and always willing to help — whether it be about classwork or career advice."
Olivia Lutterman, '22
"I want to teach high school math and physics education."
"Abstract Algebra with Professor Sara Jensen '08 was my favorite class. The workload was engaging and the friendships I made in the class were wonderful! Plus, we played with toy princesses, which was fun."
"I've been on the e-board of the Society of Physics Students (SPS) org as the treasurer since freshman year and absolutely love the group! Through SPS, I've gone to Chicago multiple times and even went to Providence, R.I. my sophomore year. We're all really friendly with everyone in the club!"
"While it was my favorite class, Abstract Algebra was also the toughest class. The content was really hard, and we were given a lot of academic independence."
Internships or on-campus employment
"My freshman year, I was an engineer on the Collegiate Rocket Launch Team through the Wisconsin Space Grant Consortium. My junior year, I was the team lead for the competition. I also tutored for the math and physics departments all four years at Carthage and was the mentor tutor for all of the math, physics, and computer science tutors.
"Off campus, I worked as an AmeriCorps science educator at the Racine Zoo and as a mechanical engineer at Los Alamos National Laboratory in New Mexico."
"I received the Hay Scholarship, Music Scholarship, and Noyce Scholarship. I'm so grateful for the scholarships I was given. I wouldn't have been able to afford Carthage without them, so I've been trying to make the best of my time in college out of respect for the money that generous donors have invested in me."
"I love hanging out with Professor Jean Quashnock during lunch and asking him endless questions about physics or hanging out in his office after hours and doing math with my classmates. I also cherish the time I spend studying with friends at Starbucks or the tutoring lounge."
"How nice everyone is!"
"If you're majoring in mathematics, be sure to get involved with academic organizations and research projects."
"I chose Carthage because of the small class sizes and its connection with the Wisconsin Space Grant Consortium."


text:
Home Tags Posts tagged with "junior"
Junior women's hockey nationals postponed due to surge in COVID-19 cases – Sports News , Firstpost
The tournament was scheduled to be held from 3 to 12 April in Simdega, Jharkhand. Representational image. Reuters New hi: The upcoming 11th junior women's hockey nationals have been postponed…
Rajiv Kapoor's performance in Toolsidas Junior is going to surprise everyone: Ashutosh Gowariker
Filmmaker Ashutosh Gowariker on Wednesday reminisced working with actor Rajiv Kapoor, who passed away on Tuesday in Mumbai. Gowariker revealed how the two bonded on the sets of sports drama…
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text:
Gamified Phishing Training Platform
Real-time Response and Analytics
For Security Teams
Just how much of a threat is Business Email Compromise?
A guide to Business Email Compromise (BEC): how it works and how you can prevent your company being a victim of the scourge of BEC
If you want to send this guide to your inbox, click here.
Cybercriminals are always looking for new and more sophisticated ways of tricking firms out of money. In the last few years, scammers have turned to a technique known as Business Email Compromise, or 'BEC'. This is a crime wave which takes social engineering to new heights. BEC can be thought of as a type of phishing: it is based on using an understanding of human behaviour to trick employees into performing the scammers' wishes. In this case, transferring money to a cybercriminal's bank account.
A recent example of the crime brings home the human as well as financial costs: an employee working in the accounts department of a British publishing house was tricked into paying out almost £200,000 GBP (around $260,000 USD)[1]. The cybercriminal behind the ruse used Business Email Compromise to achieve a successful scam. The outcome was bad for the business who lost most of the money and devastating for the employee who was sacked and subsequently sued for losing the money.
The Federal Bureau of Investigations[2] (FBI) offers some idea of the breadth and scope of Business Email Compromise:
The estimate of global costs of BEC is around $12.5 billion (USD)
S. victims have lost $2.9 billion
The number of global victims between May 2013 and May 2018 is around 78,617
Countless examples of BEC fraud exist, because this is a scam that works.
The FBI is so concerned about the explosion in BEC fraud that they have established a cross-country coordinated effort to clamp down on the crime. Operation WireWire has resulted in 74 arrests across a number of countries, but one thing can be certain: cybercriminals will not give up on a lucrative and successful tactic unless they are forced to.
Research has shown that 96 percent of companies have received BEC email scams.[3]. A report by Lloyds Bank and Get Safe Online found that 1 in 5 affected firms had to make employees redundant because of the financial impact[4].
To keep ahead of Business Email Compromise we need to understand what it is, and how the cybercriminals behind the attack operate.
What is Business Email Compromise?
BEC is a type of 'advanced deception'. It uses a sophisticated series of steps to ultimately trick someone in a company into moving money into the scammer's account. BEC is also known as CEO Fraud, because the scam often begins with the CEO – the cybercriminal placing their focus on the highest-level officers in an organization.
The cybercriminals behind the scam use the practise of social engineering. Social engineering depends on understanding and manipulating human behaviour. The BEC scammer will use a mix of surveillance and profiling techniques to understand their 'prey'. Once they have a deep knowledge of the company and who works there, they will go in for the 'kill'. At this juncture they may call upon technological techniques to augment their strategy, but sometimes they use psychology and business processes alone. To get a better idea of how a typical BEC scam works, here are the stages:
Stage One: Observing the Wildlife
The starting point for the Business Email Compromise cybercriminal is to understand who they are dealing with. This may involve using phishing emails, or simply exploring the company online. Fraudsters may even build up a rapport with company staff by emailing or calling them pretending to be a customer. This is all in the name of getting under the skin of their target – including high-ranking C-level executives.
Stage Two: Setting your Target
The cybercriminal will now create the environment that will take the scam to the next level. This may involve technology that can steal or brute force email login credentials, allowing the scammer to hijack the C-Level executive member's email account.
Alternatively, the scammer will create a spoof domain, the URL of which will look very similar to the company's domain. For example, if the target company domain is acmeincorp.com the fraudster would create a domain, acme1incorp.com. This allows them to create an email account which will look like it came from a known C-level person.
Stage Three: The Takedown
Once the cybercriminal has a good knowledge of how the company works, including the staff reporting structure, they can carry out their plan. This will typically involve sending an email using the C-level executive's account or spoof account to someone in Accounts Payable. This email will request that an urgent payment be made.
Stage Four: The Sting in the Tail
At stage one, the target person in Accounts Payable may have already been 'groomed' by the fraudster. This may have been in the form of calls or emails. It prepares them for responding to the urgent transfer request without becoming suspicious. The email they receive from the spoof C-Level executive will have several social engineering features, e.g.
It will be written in the typical style of the C-level employee (as gleaned in the surveillance stage)
It will have a sense of urgency
It will threaten a negative outcome of you do not act immediately (e.g. loss of a lucrative deal)
The Different Faces of BEC
Cybercriminals like to play with their techniques to scam business and individuals. It keeps them ahead of discovery, and Business Email Compromise is no different. There are a number of currently-known BEC techniques, such as:
Impersonation of a C-level executive or an attorney
Email account compromise
Data theft for further crimes
CEO Impersonation
Business Email Compromise is sometimes called CEO fraud or CEO impersonation as the CEO is target zero. The CEO is ultimately where the buck stops and where important decisions are made. As a trusted person within an organization, their word holds enormous weight. Coupled with this, it is an unusual employee who would query the orders of their CEO.
In CEO impersonation, the BEC fraud depends on the scammer being able to trick other company employees into believing that the scammer is the CEO. They do this by either hijacking the CEO's email account or creating a believable spoof account.
Recipients of the hijacked/spoof CEO email will then carry out the fraudsters orders as if they really were from the CEO. These orders usually take the form of sending payment to a bank account. The email will typically show the name of a known client but the account details will be changed. The money will be unknowingly sent to a bank account in the control of the cybercriminal behind the scam.
CEO Impersonation is not confined to the Chief Executive Officer. Other C-Level executives and trusted vendors such as attorneys are also under threat from BEC scammers.
A survey by Proofpoint found that 50% of compromised emails targeted the CFO and 25% targeted HR inboxes[5]. The point of the exercise is to ensure that any instructions sent by a compromised email will be taken seriously and followed through with few questions asked.
Invoice BEC
This version of BEC uses an invoice to achieve the same ends as CEO impersonation – to steal money.
The basis of this variety of BEC is, again, deception. During the surveillance stage of the BEC scam, the cybercriminal will have found their target – usually someone with authority in Accounts Payable. The scam continues using one of two techniques:
Email Compromise: The scammer will send the target employee a spear phishing email. This will harvest the login credentials of the employee's email account. The scammer keeps a watch out for incoming emails that contain an invoice. Once they find a suitable one – one with a large enough payout – they will adjust the invoice, changing the payment instructions. The invoice will be paid straight into the cybercriminal's bank account.
Email Spoof: The target this time is the company vendor list. A vendor is carefully chosen during the surveillance stage. This uses the same technique as the CEO impersonation method, i.e. the email account of the target is spoofed. An invoice is then sent out from the spoofed account purporting to be this known vendor. The invoice is attached to an email address so similar to the legitimate vendor that it gets past most checks and the payment is sent to the cybercriminal's bank account.
W2 scams and BEC
The W2 forms used by the IRS in the U.S. are the target of another version of BEC fraud. W2 forms are used by employers to record employee data. In this variant on a BEC attack, the fraudster will pose as a C-level executive and send an email requesting that they are sent the company's W2 form list. The fraudsters then use this data to commit tax fraud.
Some Examples of BEC at Work
Sometimes the best way to understand something is to look at examples. There are many BEC victims; these are a few of the most well-known:
Mattel: The toymaker handed over $3 million USD during a BEC attack. The spoof email was part of a CEO impersonation scam.[6]
Austrian company FACC Operations GmbH: This was a case of CEO impersonation. Walter Stephan, the CEO of the Austrian company[7], was sacked after the organization lost $47 million due to a BEC scam.
17 different Dallas firms were scammed out of $600,000 in total by a sophisticated CEO impersonation BEC scam. The basis of the scam was the use of spear phishing emails, which were used to compromise email accounts.[8]
Belgian bank Crelan: A total of 70 million euros was lost due to CEO impersonation.[9]
Xoom: A full $30.8 million was lost to employee impersonation where a number of spoof emails were sent making requests to the finance department to pay invoices.[10]
How Security Awareness Training Can Help Prevent Your Company Becoming a BEC Victim
Business Email Compromise is a worrying trend in sophisticated socially-engineered attacks against businesses. BEC affects organizations of all sizes and types. To counter the threat of a Business Email Compromise, no matter what type, we need to be prepared. Here are 5 ways of making sure your organization remains protected against a BEC attack:
Security awareness training for all
The best way to deal with cybersecurity issues is to know what you're up against. Security awareness training is a package of tailored education that ensures your staff are knowledgeable about a variety of cybersecurity-related areas. Packages usually include phishing simulations. These are controlled phishing exercises that are set up to mimic the types of phishing threats that your organization could encounter. Programs that use automation and gamification when developing these phishing simulations have excellent employee take-up and engagement. The phishing simulations train your employees to spot the signs of a phishing email. These sessions can be enhanced using tools like video training exercises to help staff understand the kind of tricks that a BEC scammer would use to carry out the scam.
Take control of your company domain and similar names
BEC fraudsters will often buy up domain names similar to their target's domain. For example, if your company name is myapple.com a fraudster might buy the domain miapple.com or myapp1e.com
Make sure that your company purchases any domain names similar to your company URL.
Operational procedure changes
Carry out a risk assessment on any procedure that may be compromised in a BEC attack. For example, does your firm double-check financial movement requests over a certain amount? If risks are identified in any areas that could be exploited in a BEC attack, find procedural ways to close the gap. This could be as simple as requiring a phone call check – to a recipient's verified number – before submitting payment for an invoice.
Robust email authentication
Some BEC attacks are based on compromising the email of a target person such as a C-level executive. Most email system now allow you to set up a second factor to authenticate access to the account. Second factors are usually applied after a person enters their username and password. They are typically something like a mobile authenticator app or an SMS text code.
Good patch hygiene and anti-malware
Phishing, often a key part of a BEC attack, also comes in several flavors. This includes possible infection of a target computer with malware such as keyloggers. This type of malware collects keystrokes from a keyboard; this enables it to steal login credentials and other sensitive data. Malware infection is usually dependent on software flaws. One way to reduce the chances of infection is to make sure that all software is fully up-to-date and that security patches are applied promptly. Using anti-malware applications as part of a wider security strategy, including security awareness training, also helps mitigate the risk of infection.
All businesses need to be aware of Business Email Compromise, and take the risk of falling foul of this crime very seriously. The scam is costing organizations money – sometimes millions of dollars – and employee loss on a huge global scale. For individuals unwittingly taken in by BEC scams, the impact on their lives and livelihoods can be catastrophic . BEC fraud is much more than a 'hit and run' crime like ransomware. It is insidious, the cybercriminals taking their time to survey their target, understand their business, and spoof or steal their email accounts. It is a crime where the cybercriminal really gets under the skin of the business it wants to extract money from.
In the case of BEC fraud, the best start is to understand what you are dealing with. Being BEC aware across your organization is the foundation stone to taking on the cybercriminals and winning. Having a security awareness training program that creates a culture of security and knowledge will help you to stop BEC crime in its tracks. Adding to this arsenal, technological control in the form of domain protection and robust authentication is also important as part of an overall BEC prevention strategy.
Cybercrime like BEC is no game. It is a serious attack on the very heart of your organization, your people and your finances. Fortunately, we have the means to tackle this growing threat at our fingertips by making our staff BEC aware.
About Hoxhunt
Hoxhunt turns your employees to your strongest asset in cyber security. We're relentlessly focused on empowering your employees to shield your organisation as an active last line of defence. We work with multinational companies such as Friesland Campina, Konecranes, Nest and Nokia. If you want to see how we can help your company defend against attacks such as BEC, request a demo at hoxhunt.com or contact us at [email protected].
Learn about the latest trends and news in social engineering and phishing.
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Q: How to retrieve data from firebase and compare the data with string in Javascript? I'm not very used to Javascript code and firebase.
So, in firebase I have one parent node where I need to get the data from. This parent has child where each child has two kind of value in it (refer to the image)

Firstly I need to compare if my "Tanda" value equals to "ada kebakaran". If it's equal, then it start to retrieve the value on "kode".
this "kode" is use as reference to get more data in another parent node.
so far my code like this
function getdata(data){
firebase.database().ref("sensor").on('value', function(snapshot)){
  snapshot.forEach(function(childSnapshot))
  {
    var sensor = childSnapshot.val();
    var keys = Object.keys(sensor);
    for (var i = 0; i < keys.length; i++){
      var k = keys[i];
      var tanda = sensor[k].tanda;
      if(tanda && "ada kebakaran"){
        //get the "kode" here

A: You need to do the following:
firebase.database().ref("sensor").on('value', function(snapshot)){
  snapshot.forEach(function(childSnapshot))
  {
    var sensor = childSnapshot.val();
    var tanda  = sensor["tanda_kebakaran"];
      if(tanda == "ada kebakaran"){
        //get the "kode" here
        var kode = sensor.kode;
       }
    });

Add a reference to node sensor then iterate using forEach(), childSnapshot.val() will contain all the data under sensor.. Then you can access tanda_kebakaran value using bracket notation, and compare it.

A: Pardon me if I understood the question differently.
From what I understood, here's the code.
admin.firestore().collection("sensor").get().then((data) => {
    let finalData = [];
    data.forEach((doc) => {
        if(doc.tanda_kebakaran === "1")
            finalData.push({
                kode: doc.kode,
                tanda_kebakaran: doc.tanda_kebakaran
            });
    })
})

the finalData array should have the data you need.


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Our Blog - SCHILLER Australia tagged "Study"
Finally, some good news: you can turn your health around, even once you've reached middle-age.
With the help of 3D printing, combined with other more traditional methods of examination, Doctors at the Henry Ford Hospital in Detroit are conquering difficult operations that were once prone to postoperative complications.
Apple has, just this week, launched an Apple Heart Study with the release of the Heart Study app. All you need is an Apple Watch and an iPhone to participate.
Hypertension: with increasing prevalence, it is now a major health concern all over the world. And sleep could help you prevent suffering from it!
According to a recent study, e-cigarettes may impair heart muscle function.
ECG tests for heart attacks are widely considered the norm, but recent studies out of London suggest that a simple blood test may be a more effective option for detection and swift treatment.
Want to know how well you are REALLY ageing? Read on!
Need an Ultrasound? There's an app for that!
A recent clinical trial has demonstrated that the camera on your smartphone can noninvasively provide detailed information about your heart's health.
Is standing the new smoking?
Stand-up desks have taken off recently as part of a new trend to promote healthy living and prevent workers from sitting for an entire work shift. However, it is now believed that predominantly standing all day can in fact have a detrimental effect on people's health.
A drug that fights inflammation can reduce the risk of heart attacks and strokes in people who have already had one heart attack and are at high risk for another, a new study finds.
Could this be the Gold standard in wearables?
With an aim to reduce the bulky health sensors that are currently used by practitioners, scientists have created a super-thin wearable that has the ability to record data through skin.
As a response to the soaring numbers of individuals that suffer from addiction to prescription medication, one clinical trial is trying to alleviate the need for drugs such as fentanyl for back pain in particular.
Have you been feeling stressed lately? A recent study suggests there is one key thing you can do this afternoon to help!
The former president of the World Heart Federation has recently warned that guidelines on salt intake are too low and may be increasing your risk of a fatal heart attack.
Dear Women, you need more sleep!
All the tired ladies: it's official, you don't need to be sorry for needing more sleep than your male counterparts!
A recent study suggests you might just be at risk of health problems if you happen to overindulge in the not-so-good stuff.
Are your painkillers killing you?
As a consumer, you're probably aware of some of the side effects of your common over-the-counter pain killers. You take precautionary methods to protect yourself, such as only ever taking ibuprofen with food to avoid stomach ulcers. But what about the side effects you can't prevent with a little lining of the stomach?
The new research is set to help patients who have suffered a heart attack or genetic defects by helping to replace damaged tissues through new growth.
Following his breakthrough realisation, Parker returned to his lab with the view to build a jellyfish-inspired robot, powered by muscles made of living heart cells from a rat.
With another positive outcome from a recent study, a glass of red wine receives a big tick as apart of a healthy lifestyle.
Recent research in America and Australia has found that we may need to tighten blood pressure guidelines to further reduce the risk of stroke, heart failure & kidney disease.


Growing up in the 70s and 80s, it was impossible not to feel the impact that the oil and natural gas industry had on southern Louisiana. Local businesses boomed with money from oil profits. Most people I knew had some connection to the industry, either by working in the oil field, or in one of its many support industries. Working offshore was one of the best paying jobs in southern Louisiana for a non-college graduate. In fact, you could make a lot more money working offshore than most college graduates could. My grandfather worked on an Exxon drilling platform for 40 years, and was able to comfortably support his wife and six children on his salary. Sadly, he was part of the last generation of Cajuns who could work in the oil field for 40 years, and get the gold watch treatment.
Oil played a huge role in Louisiana in the 20th century. Land based oil exploration began in Louisiana in the early 1900s, and the first offshore platform was built off the Louisiana coast in the 1940s. Many thousands of Cajun men were drawn to this industry in the years that followed. When oil and gas prices rose in the 1970s, Louisiana's economy boomed. Oil companies built more rigs and hired more people on the assumption that the price of oil would reach $50 a barrel, a bet that was lost when prices crashed to $10 a barrel in the mid 1980s. In the aftermath of the crash, unemployment reached double digits and Louisiana residents experienced a deep recession, with many people losing their livelyhoods. While the rest of the country enjoyed a booming economy, the 1980s was a hard time for Louisiana and its citizens.
Most offshore workers work one of two types of shifts, a 7 & 7, or a 14 & 7, meaning 7 days working followed by 7 days off or 14 days working and 7 days off. I spent a summer working on a natural gas platform, and I can easily say it's the hardest job I ever worked. I'd wake up at 4am every other Monday morning and drive out to Intracoastal City, deep in Vermilion Parish. There I'd take a 45 minute helicopter ride out to my platform with my co-workers. Once I arrived, I was put right to work. As low man on the totem poll, I was stuck doing most of the menial tasks, from unloading the supply boats, to sandblasting and painting the rig while dangling 150 ft over the water. At the end of a hard 12 hour day, I wound down as most roughnecks do, by eating lots of food, watching TV, and playing some cards or pool at night.
Life on a rig is full of all sorts of potential hazards. It's very easy to lose a finger or toe, get struck by a heavy object, or throw your back out lifting something heavy. The risk of injury is multiplied by the remoteness of the rig. Any hospital emergency room is well over an hour away, and rig staff usually have minimal first aid training. Injuries are so common, in fact, that local law firms have created a cottage industry of offshore injury litigation. Sure, your back might not work again, but you'll have the best bass boat in the neighborhood while you collect workman's comp. Luckily, I survived my summer offshore with no injuries, but I'm convinced that had I stayed longer, it was just a matter of time before something happened to me.
Today, Louisiana remains the #1 producer of crude oil, and #2 producer of natural gas in the United States. With 19 operating crude oil refineries, it has the second largest refining capacity in the US. Louisiana supplies a quarter of the U.S. production of natural gas. There are currently more 2,300 active oil and gas platforms in the Gulf of Mexico. With oil prices over $110 a barrel, the industry is once again booming, though not at the same levels seen in the 1970s. There are many jobs to go around, but people who lived through the last recession are reluctant to return since they fear that there's no long term future in the field. Fool me once, shame on you. Fool me twice, shame on me.
This entry was posted in Culture, Louisiana, Outdoors, Work and tagged Cajun, Drilling, Gulf of Mexico, Industry, Louisiana, Natural Gas, Offshore, Oil Crash, Oil Rig. Bookmark the permalink.
About 75% of the boys I know from back home work or have worked off shore, including 2 of my brothers.
You must have grown up pretty close to the gulf then.
My pawpaw worked and retired from Exxon. My daddy worked offshore and my husband did, too. Now they both do heat treating.
What are the jobs like now for someone coming in from out of state to work off shore? Possibly a galley hand or unskilled (as far as the oil business goes) type of work.
No idea. I haven't lived in Louisiana for 10 years. With no experience, you pretty much have to work your way up from the bottom, and hope the bottom doesn't fall out of the oil market and leave you unemployed. There are several high paying dangerous jobs out there like underwater welding, diving, etc. Those pay pretty well, if you don't get killed first.
I have been welding for a while now, and i do pretty well paywise…but I wanted to get into the underwater welding scene…Does anyone have recommendations for a company that I could look into and/or specific locations of where I should look. Right now, I'm considering an underwater weld program, one in Jacksonville Florida and the other in San Diego California…I was also wondering, lets say I got a job at Exxon or BP or something along those lines, would they pay for the dive training??
I have been working offshore for the past few years. The only time i dont feel safe is on the chopper. one thing about offshore your either a coonass (Louisiana) or a redneck (Texas) plenty of people from Mississippi but who knows where they fall?
I've been in the buisness since 1970 and it's great. The jobs have gotten a lot safer than when I started. The buisness is slow now, but it will pick up again soon. Ilove the 14 and 14 work schedule.
I started working on my dad's crew during the summer as soon as I turned 16 (But even before I turned of age, my dad would take me down during the summer just to hang out). I even spent time on a land crew up in Oklahoma and Arkansas. Em was some good times-The boat was sometimes parked at some tiny dock with access to a road-I did alot of underage drinking back there. In LA we worked down near Grand Isle, Sabine Wildlife Preserve, and Cocodrie. Sabine had alligators every 4 ft down the canal and we had a monster 13fter that we feed every day. Cocodrie had nutria the buggies used to run over-we never saw them until it was too late. Got to drive and ride crew boats, marsh buggies and airboats, got to spend all day outside (being stuck in the cane breaks was not fun—no air whatsoever) swim in the gulf, catch gators when we were bored and all the food you can eat-no charge!
I agree with you Working offshore was one of the best paying jobs in the world but with big risks.


The Daylesford and Hepburn Springs area has a natural beauty that must be seen anyway you can - walking, running, cycling or driving.
If you are touring make sure you get out of the car and take in the fresh air and stunning scenery. Go for a walk and have a close up look - you will be amazed!
Catching a fish is guaranteed, if you want we can even cook it up for you.
Have fun and enjoy the stunning farmland scenery.
Wombat Hill Botanic Gardens - very old stunning gardens with cafe.
Lake Daylesford Pedal Pushers Boat Hire - 2 Leggatt St, Daylesford.


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Jay Blogs – What Does Love Require?
by Karolyn Davis | Oct 31, 2019 | Classical School News, Elementary School News, High School News, Jay's Blog, Junior High News, News | 0 comments
I had a friend ask me a question the other day regarding an issue involving a student situation, and how to handle it. The question has been haunting me ever since: "What does love require?" As Christians, we know we're called to love. Jesus' Great Commandment is, simply, to love, "Love the Lord your God with all your heart, soul, mind, and strength, and love your neighbor as yourself." (Matt. 22:37). But, what does love really mean? What does love actually require?
Matt Chandler once observed that we use "love" to capture many ideas: I love my wife; I love the Baylor Bears; I love salted caramel ice cream; I love Jesus. Love can't mean the same thing to capture all those sentiments. To actually love with a God-shaped calling can't mean the same thing as "have an affinity for," "prefer," or "be attracted to," and still capture Christ's command to love. We can't conflate all these ideas when we say "love." Love, as Christ calls us to love, is not a feeling or a preference; it's a willful act.
Love is the conscious decision to be all for another. If so, what does love actually require?
Anyone who has actually ever truly loved knows that love requires suffering. In his wonderful book, A Loving Life, Paul Miller says that "suffering is the crucible for love." Counterfeit love is full of all sorts of self-interest, and stems from a desire to have one's needs met, even at another's expense. Suffering is the place where self comes to die, where we're stripped down to the state of humility that allows us to truly love. To love is to suffer.
Suffering also requires sacrifice. In fact, the true measure of love is what you're willing to give up for it. The pure love of a parent is willing to sacrifice everything, and expects (and often receives) nothing in return. The ultimate love of our Father in Heaven conquered death through the shed blood of His son, love that cost Him everything.
Perhaps the greatest passage on love in Scripture is found in I Corinthians 13, Paul's famous "love" chapter. Ironically, we read it most often in the context of marriage and weddings; however, Paul wrote it for the church, a group of people called to unity through loving each other and using its gifts to serve each other. This kind of love is not eros, not romantic love, but phileo, brotherly love. It's how we're to love God and love our neighbor.
Love is patient, and kind, and doesn't insist on its own way. It's not irritable or resentful. This kind of love is built for daily living, and daily loving. As chapter 13 says, it bears all things, believes all things, hopes all things, endures all things. It is relentless and persevering, even when it doesn't want to be.
So what does love require? Love requires a desire to tell others about the way to eternal life. Entertainer Penn Gillette, who is not a believer, once famously said, "How much do you have to hate someone when you believe you know the only way to be saved from death, and you fail to tell them about it?" Even Gillette understood that love isn't afraid of offense, or is strong enough to conquer that fear. We're preconditioned by a dark culture that doesn't want us to tell the world about Jesus, tells us that doing so is offensive, a social faux pas, not for polite company at best, a violent act at worst. But, love requires breaking through social mores to others' deepest need, whether or not they're aware of that need.
Love requires being the one to initiate the resolution of conflict. Love requires the act of kindness to the person who treated you like dirt. Love requires the tempered response to the person who just blasted you on email or social media. Love requires choosing to ascribe good intentions to the person who just said or did something whose word or act could be interpreted either way. Love requires giving one more chance. Love requires walking across the room and introducing yourself to or engaging that person, even if that person is completely "other" than you. Love requires gathering those moms and dads who you don't really know that well together for prayer. Love requires a commitment to peace–not fake peace, which is just ignoring problems and conflict, but doing the hard work of confronting, humbling oneself to admitting wrong, trying to see things through other's eyes, and seeking and extending forgiveness.
So much of love is unnatural, which is why it requires drawing on supernatural strength, pressing into the Lord daily for strength and grace, humility and perseverance. Love requires staying in the fight, and never letting go.
Love is the most powerful force on earth. When set even against the second most powerful force, death, love won. And, we can't fully live without it. Love requires all that we are, and all that we have. Yet, it gives everything in return, even when we don't expect it. And, we can't do the "community" part of Grace Community School without it.
Jay Ferguson, PhD, Head of School at Grace Community School, writes regularly on his blog, JaysBlog.org.
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