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Trösztellenes eljárás folyik a Meta ellen, lehet, hogy el kell adnia az Instagramot Telex 2025-04-14 09:45:38 Mobiltech Instagram A Szövetségi Kereskedelmi Bizottság szerint a cég monopóliumot szerzett azzal, hogy felvásárolta az Instagramot és a WhatsAppot is a Facebook mellé. Tényleg realitás a kihalt fajok feltámasztása? 24.hu 2025-04-14 15:00:54 Tudomány Végigsöpört a világsajtón a szenzációs hír: a Colossal Biosciences nevű vállalatnak sikerült feltámasztania egy kihalt, jégkori ragadozót. Mit gondol a szakma a projektről? Fiataloknak szóló vállalkozói műsor indul, ahol 10 millió forinttal lehet gazdagabb a nyertes refresher.hu 2025-04-14 15:45:00 Tudomány A versenybe a jó vállalkozói ötlettel rendelkező, ambiciózus fiatalok jelentkezését várják. Cipőt a cipőboltból, podcastet a YouTube-ról HWSW 2025-04-14 12:23:30 Infotech YouTube A magyarok elsöprő többsége a YouTube-on hallgat podcasteket, a műfaj egyre népszerűbb, az elköteleződés azonban nem jellemző a hallgatók körében. Váratlan támogatókat talált Elon Musk az OpenAI elleni peréhez IT café 2025-04-14 09:52:00 Infotech Mesterséges intelligencia Elon Musk OpenAI Az OpenAI korábbi alkalmazottai közül többen is Elon Musk mellé álltak a cég elleni perben. Hirtelen sokan kezdtek el autonóm tengeri hajókat fejleszteni SG.hu 2025-04-14 13:27:49 Tudomány Szilícium-völgy A Szilícium-völgy növekvő védelmi iparának új célja a legénység nélküli hadihajó. Korlátozni fogja a YouTube, hogy mennyi rövid videót nézünk rajta PC Fórum 2025-04-14 08:30:00 Mobiltech Google YouTube A Google a jelek szerint egy olyan új fejlesztés bevezetését tervezi YouTube alkalmazásába, ami korlátozná azt, hogy mennyi rövid videót nézhetünk meg abban. Ugyanakkor ezt a korlátot nem maga a keresőóriás állítaná be, hanem mi magunk, az app felhasználói határozhatnánk meg. Molekulafelhő a Perseusban Csillagászat 2025-04-14 07:31:39 Tudomány Varga István Az LBN 640 (Lynds Catalog of Bright Nebulae) egy ritkán fotózott objektum a Perseus csillagképben: egy ív alakú molekulafelhő, csúcsán egy kis reflexiós köddel, ami egyben OIII-ban sugárzó csillagkeletkezési régió is. Varga István, Cserszegtomaj Kialakulásáért a nagyjából 6000 fényévre lévő Perseus OB1 csillagtársulás felelős, aminek középső régi Legalább 50 éve velünk vannak a mikroműanyagok Qubit 2025-04-14 09:37:12 Tudomány Hollandia Egy 1971-ben gyűjtött édesvízi rovarlárva lakócsövében építve találtak műanyagot a hollandiai Naturalis Biodiverzitási Központ kutatói. Az újabb képgeneráló AI-funkciók tovább növelik a szerzői jogi aggályokat digitrend-i 2025-04-14 10:42:11 Infotech Mesterséges intelligencia ChatGPT A mesterséges intelligencia(AI) alapú eszközök használatánál kezdettől fogva felmerültek a különféle szerzői jogokkal kapcsolatos aggályok, legyen szó szöveges tartalomról vagy képekről. Még fontosabb erre odafigyelnünk a ChatGPT nemrégiben bevezetett új képgeneráló funkciója után. Szakértői tanácsok mire vigyázzunk. A „ChatGPT Studio Ghibli” kifej Égi jelenségek 2025. április második felében National Geographic 2025-04-14 07:50:04 Tudomány Világűr Korán kelők újra láthatják a Vénuszt, búcsúzunk a téli csillagképektől, számos együttállás és holdsarló látványa kényezteti az églesőket, és érkezik az év első jelentős meteorraja is. A Chicxulub-kráter – Egy becsapódás, amely megváltoztatta a Föld történetét PlanetZ 2025-04-14 10:17:57 Tudomány Világűr Meteor Ismerd meg a Föld múltjának sorsfordító pillanatát! A Chicxulub-kráter egy ősi aszteroida-becsapódás nyoma, amely a dinoszauruszok kihalását okozta. A Schaeffler a humanoid robotok kulcstechnológiáira épít autopro 2025-04-14 04:21:00 Gazdaság Németország Kiállítás Robot A Schaeffler a Hannover Messe kiállításon mutatta be kulcskomponenseit a humanoid robotok számára. A további adásainkat keresd a podcast.hirstart.hu oldalunkon.
Trösztellenes eljárás folyik a Meta ellen, lehet, hogy el kell adnia az Instagramot Telex 2025-04-14 09:45:38 Mobiltech Instagram A Szövetségi Kereskedelmi Bizottság szerint a cég monopóliumot szerzett azzal, hogy felvásárolta az Instagramot és a WhatsAppot is a Facebook mellé. Tényleg realitás a kihalt fajok feltámasztása? 24.hu 2025-04-14 15:00:54 Tudomány Végigsöpört a világsajtón a szenzációs hír: a Colossal Biosciences nevű vállalatnak sikerült feltámasztania egy kihalt, jégkori ragadozót. Mit gondol a szakma a projektről? Fiataloknak szóló vállalkozói műsor indul, ahol 10 millió forinttal lehet gazdagabb a nyertes refresher.hu 2025-04-14 15:45:00 Tudomány A versenybe a jó vállalkozói ötlettel rendelkező, ambiciózus fiatalok jelentkezését várják. Cipőt a cipőboltból, podcastet a YouTube-ról HWSW 2025-04-14 12:23:30 Infotech YouTube A magyarok elsöprő többsége a YouTube-on hallgat podcasteket, a műfaj egyre népszerűbb, az elköteleződés azonban nem jellemző a hallgatók körében. Váratlan támogatókat talált Elon Musk az OpenAI elleni peréhez IT café 2025-04-14 09:52:00 Infotech Mesterséges intelligencia Elon Musk OpenAI Az OpenAI korábbi alkalmazottai közül többen is Elon Musk mellé álltak a cég elleni perben. Hirtelen sokan kezdtek el autonóm tengeri hajókat fejleszteni SG.hu 2025-04-14 13:27:49 Tudomány Szilícium-völgy A Szilícium-völgy növekvő védelmi iparának új célja a legénység nélküli hadihajó. Korlátozni fogja a YouTube, hogy mennyi rövid videót nézünk rajta PC Fórum 2025-04-14 08:30:00 Mobiltech Google YouTube A Google a jelek szerint egy olyan új fejlesztés bevezetését tervezi YouTube alkalmazásába, ami korlátozná azt, hogy mennyi rövid videót nézhetünk meg abban. Ugyanakkor ezt a korlátot nem maga a keresőóriás állítaná be, hanem mi magunk, az app felhasználói határozhatnánk meg. Molekulafelhő a Perseusban Csillagászat 2025-04-14 07:31:39 Tudomány Varga István Az LBN 640 (Lynds Catalog of Bright Nebulae) egy ritkán fotózott objektum a Perseus csillagképben: egy ív alakú molekulafelhő, csúcsán egy kis reflexiós köddel, ami egyben OIII-ban sugárzó csillagkeletkezési régió is. Varga István, Cserszegtomaj Kialakulásáért a nagyjából 6000 fényévre lévő Perseus OB1 csillagtársulás felelős, aminek középső régi Legalább 50 éve velünk vannak a mikroműanyagok Qubit 2025-04-14 09:37:12 Tudomány Hollandia Egy 1971-ben gyűjtött édesvízi rovarlárva lakócsövében építve találtak műanyagot a hollandiai Naturalis Biodiverzitási Központ kutatói. Az újabb képgeneráló AI-funkciók tovább növelik a szerzői jogi aggályokat digitrend-i 2025-04-14 10:42:11 Infotech Mesterséges intelligencia ChatGPT A mesterséges intelligencia(AI) alapú eszközök használatánál kezdettől fogva felmerültek a különféle szerzői jogokkal kapcsolatos aggályok, legyen szó szöveges tartalomról vagy képekről. Még fontosabb erre odafigyelnünk a ChatGPT nemrégiben bevezetett új képgeneráló funkciója után. Szakértői tanácsok mire vigyázzunk. A „ChatGPT Studio Ghibli” kifej Égi jelenségek 2025. április második felében National Geographic 2025-04-14 07:50:04 Tudomány Világűr Korán kelők újra láthatják a Vénuszt, búcsúzunk a téli csillagképektől, számos együttállás és holdsarló látványa kényezteti az églesőket, és érkezik az év első jelentős meteorraja is. A Chicxulub-kráter – Egy becsapódás, amely megváltoztatta a Föld történetét PlanetZ 2025-04-14 10:17:57 Tudomány Világűr Meteor Ismerd meg a Föld múltjának sorsfordító pillanatát! A Chicxulub-kráter egy ősi aszteroida-becsapódás nyoma, amely a dinoszauruszok kihalását okozta. A Schaeffler a humanoid robotok kulcstechnológiáira épít autopro 2025-04-14 04:21:00 Gazdaság Németország Kiállítás Robot A Schaeffler a Hannover Messe kiállításon mutatta be kulcskomponenseit a humanoid robotok számára. A további adásainkat keresd a podcast.hirstart.hu oldalunkon.
Oiii, querido(a). Como é que você tá? Trouxe este episódio bem no final do ano para que seu sofrimento não aumente ao escutar as ideias sobre final de ano e metas e etc. Espero que te faça sentido. Te convido a me acompanhar no Instagram @psithalitacouto
Descriçaaaaaawwwwww: Oiii gente! No EP de hoje nós estamos brincando de; “Quem é mais provável?”, onde citamos inúmeras situações que podem ou não acontecer e quem de nós três se identifica mais com elas. Ahhh esse EP também está disponível em vídeo pra vocês acompanharem nossas votações com as plaquinhas. IG do Podcast: @falagaypodcast | E-mail: falagaypodcast@gmail.com Hosts: @cleytonleite8 | @davidcsta @hiroshitakeuti --- Send in a voice message: https://podcasters.spotify.com/pod/show/falagaypodcast/message
MOSEL Survey: Extremely weak outflows in EoR analogues at z=3-4 by Anshu Gupta et al. on Monday 28 November This paper presents deep K-band spectroscopic observations of galaxies at z=3-4 with composite photometric rest-frame Hb+[OIII] equivalent widths EW_0>600A, comparable to the EW of galaxies observed during the epoch of reionisation (EoR, z>6). The typical spectroscopic [OIII] EW_0 and stellar mass of our targets is ~ 700A and log(M_star/M_sun)=8.98. By stacking the [OIII] emission profiles, we find evidence of a weak broad component with F_broad/F_narrow ~ 0.2 and velocity width sigma_{broad} ~ 170 km/s. The strength and velocity width of the broad component does not change significantly with stellar mass and [OIII] EW_0 of the stacked sample. Assuming similar broad component profiles for [OIII] and Halpha emission, we estimate a mass loading factor ~0.2, similar to low stellar mass galaxies at z>1 even if the star formation rates of our sample is 10 times higher. We hypothesize that either the multi-phase nature of supernovae driven outflows or the suppression of winds in the extreme star-forming regime is responsible for the weak signature of outflows in the EoR analogues. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.13763v1
MOSEL Survey: Extremely weak outflows in EoR analogues at z=3-4 by Anshu Gupta et al. on Sunday 27 November This paper presents deep K-band spectroscopic observations of galaxies at z=3-4 with composite photometric rest-frame Hb+[OIII] equivalent widths EW_0>600A, comparable to the EW of galaxies observed during the epoch of reionisation (EoR, z>6). The typical spectroscopic [OIII] EW_0 and stellar mass of our targets is ~ 700A and log(M_star/M_sun)=8.98. By stacking the [OIII] emission profiles, we find evidence of a weak broad component with F_broad/F_narrow ~ 0.2 and velocity width sigma_{broad} ~ 170 km/s. The strength and velocity width of the broad component does not change significantly with stellar mass and [OIII] EW_0 of the stacked sample. Assuming similar broad component profiles for [OIII] and Halpha emission, we estimate a mass loading factor ~0.2, similar to low stellar mass galaxies at z>1 even if the star formation rates of our sample is 10 times higher. We hypothesize that either the multi-phase nature of supernovae driven outflows or the suppression of winds in the extreme star-forming regime is responsible for the weak signature of outflows in the EoR analogues. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.13763v1
MASCOT: Molecular gas depletion times and metallicity gradients -- evidence for feedback in quenching active galaxies by C. Bertemes et al. on Thursday 24 November We present results from the first public data release of the MaNGA-ARO Survey of CO Targets (MASCOT), focussing our study on galaxies whose star-formation rates and stellar masses place them below the ridge of the star-forming Main Sequence. In optically-selected type 2 AGN/LINERs/Composites, we find an empirical relation between gas-phase metallicity gradients $nabla Z$ and global molecular gas depletion times $t_mathrm{dep} = M_{H_2}$/SFR with "more quenched" systems showing flatter/positive gradients. Our results are based on the O3N2 metallicity diagnostic (applied to star-forming regions within a given galaxy) which was recently suggested to also be robust against emission by diffuse ionised gas (DIG) and low-ionisation nuclear emission regions (LINERs). We conduct a systematic investigation into possible drivers of the observed $nabla Z$ - $t_mathrm{dep}$ relation (ouflows, gas accretion, in-situ star formation, mergers, and morphology). We find a strong relation between $nabla Z$ or $t_mathrm{dep}$ and centralised outflow strength traced by the [OIII] velocity broadening. We also find signatures of suppressed star-formation in the outskirts in AGN-like galaxies with long depletion times and an enhancement of metals in the outer regions. We find no evidence of inflows impacting the metallicity gradients, and none of our results are found to be significantly affected by merger activity or morphology. We thus conclude that the observed $nabla Z$ - $t_mathrm{dep}$ relation may stem from a combination of metal redistribution via weak feedback, and a connection to in-situ star formation via a resolved mass-metallicity-SFR relation. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12518v1
MASCOT: Molecular gas depletion times and metallicity gradients -- evidence for feedback in quenching active galaxies by C. Bertemes et al. on Wednesday 23 November We present results from the first public data release of the MaNGA-ARO Survey of CO Targets (MASCOT), focussing our study on galaxies whose star-formation rates and stellar masses place them below the ridge of the star-forming Main Sequence. In optically-selected type 2 AGN/LINERs/Composites, we find an empirical relation between gas-phase metallicity gradients $nabla Z$ and global molecular gas depletion times $t_mathrm{dep} = M_{H_2}$/SFR with "more quenched" systems showing flatter/positive gradients. Our results are based on the O3N2 metallicity diagnostic (applied to star-forming regions within a given galaxy) which was recently suggested to also be robust against emission by diffuse ionised gas (DIG) and low-ionisation nuclear emission regions (LINERs). We conduct a systematic investigation into possible drivers of the observed $nabla Z$ - $t_mathrm{dep}$ relation (ouflows, gas accretion, in-situ star formation, mergers, and morphology). We find a strong relation between $nabla Z$ or $t_mathrm{dep}$ and centralised outflow strength traced by the [OIII] velocity broadening. We also find signatures of suppressed star-formation in the outskirts in AGN-like galaxies with long depletion times and an enhancement of metals in the outer regions. We find no evidence of inflows impacting the metallicity gradients, and none of our results are found to be significantly affected by merger activity or morphology. We thus conclude that the observed $nabla Z$ - $t_mathrm{dep}$ relation may stem from a combination of metal redistribution via weak feedback, and a connection to in-situ star formation via a resolved mass-metallicity-SFR relation. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12518v1
O3 Mining Inc. is a gold exploration and development company focused on its assets located in Québec, Canada. The company's Marban Engineering Gold project is located approximately 15 km west of the town of Val-d'Or in the Abitibi-Temiscamingue region of Quebec, Canada. The project is a 1,023-hectare land package, consisting of approximately 30 mining claims and three mining concessions.
Polar Dust Emission in Quasar IR SEDs and Its Correlation with Narrow Line Regions by Jianwei Lyu et al. on Monday 17 October Polar dust has been found to play an important role in the mid-infrared emission of nearby Seyfert nuclei. If and how often polar dust exists among the quasar population is unknown due to the lack of spatially-resolved observations. In this Letter, we report correlations between the prominence of AGN forbidden line emission (commonly associated with the narrow line region) and the dust mid-IR energy output among the archetypal Palomar-Green quasar sample and other bright type-1 AGNs drawn from the SDSS, Spitzer and WISE archives. The AGN mid-IR color differences traced by WISE W2 ($sim4.6 mu m$)$-$W3 ($sim12 mu m$) and W2 ($sim4.6 mu m$)$-$W4 ($sim22 mu m$), and near-IR to mid-IR SEDs constrained with 2MASS, WISE and Spitzer data have clear trends with the relative strength of the forbidden line regions traced by the optical OIII and mid-IR OIV emission lines. These observations indicate that, where the lines are strong, a large fraction of the AGN emission at $lambdagtrsim5 mu$m comes from dust in the forbidden line regions. We find that the widely quoted universal AGN template is a result of averaging quasar SEDs with different levels of polar dust emission above the torus output and that the typical intrinsic IR SED of compact torus dust emission alone falls with increasing wavelength past 5 $mu$m (in $nu F_nu$). In addition, the association of polar dust with the forbidden lines suggests an alternative to the receding torus hypothesis for the decrease in infrared output with increasing AGN luminosity. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.08037v1
ALMA Observation of a z gtrsim10 Galaxy Candidate Discovered with JWST by Ilsang Yoon et al. on Monday 17 October We report ALMA observation of a $zgtrsim10$ galaxy candidate (GHZ1) discovered from the GLASS-JWST Early Release Science Program. Our ALMA program aims to detect the [OIII] emission line at the rest-frame 3393.0062 GHz ($88.36mu$m) and far-IR continuum emission with the spectral window setup seamlessly covering 26.125 GHz frequency range ($10.10
Oiii genteee, no último devocional conversamos sobre "COMPARAÇÃO" e hoje vamos dar continuidade nesse tema abordando sobre "CONTENTAMENTO". Quando abandonamos a comparação, entramos em um estado de contentamento que é a alegria e satisfação em nossa própria jornada com Cristo. Quando entendemos a nossa identidade em Cristo, nos tornamos satisfeitas com aquilo que Ele tem feito em nós e por nós. Eu quero sabeeer, conta pra mim nos comentários o que Senhor tem feito na sua vida através do devocional.
On the Origin of the Strong Optical Variability of Emission-line Galaxies by Ruqiu Lin et al. on Thursday 22 September Emission-line galaxies (ELGs) are crucial in understanding the formation and evolution of galaxies, while little is known about their variability. Here we report the study on the optical variability of a sample of ELGs selected in the COSMOS field, which has narrow-band observations in two epochs separated by $gtrsim$ 12 years. This sample was observed with Suprime-Cam (SC) and Hyper Suprime-Cam (HSC) on the $Subaru$ telescope in NB816 and $i'/i$ bands, respectively. After carefully removing the wing effect of a narrow-band filter, we check the optical variability in a sample of 181 spectroscopically confirmed ELGs. We find that 0 (0/68) Ha emitters, 11.9% (5/42) [OIII] emitters, and 0 (0/71) [OII] emitters show significant variability ($|Delta m_{NB}| geq 3,sigma_{Delta m_{NB,AGN}} = 0.20, mag$) in the two-epoch narrow-band observations. We investigate the presence of active galactic nucleus (AGN) in this variable ELG (var-ELG) sample with three methods, including X-ray luminosity, mid-infrared activity, and radio-excess. We find zero bright AGN in this var-ELG sample, but cannot rule out the contribution from faint AGN. We find that SNe could also dominate the variability of the var-ELG sample. The merger morphology shown in the HST/F814W images of all the var-ELG sample is in agreement with the enhancement of star formation, i.e., the SNe activity. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.07087v2
Low-ionization structures in planetary nebulae -- II Densities, temperatures, abundances and excitation of 6 PNe by M. Belén Mari et al. on Thursday 22 September Here we present the spatially resolved study of six Galactic planetary nebulae (PNe), namely IC 4593, Hen 2-186, Hen 2-429, NGC 3918, NGC 6543 and NGC 6905, from intermediate-resolution spectra of the 2.5 m Isaac Newton Telescope and the 1.54 m Danish telescope. The physical conditions (electron densities, N$_{e}$, and temperatures, T$_{e}$), chemical compositions and dominant excitation mechanisms for the different regions of these objects are derived, in an attempt to go deeper on the knowledge of the low-ionization structures (LISs) hosted by these PNe. We reinforce the previous conclusions that LISs are characterized by lower (or at most equal) N$_{e}$ than their associated rims and shells. As for the T$_{e}$, we point out a textit{possible} different trend between the N and O diagnostics. T$_e$[NII] does not show significant variations throughout the nebular components, whereas T$_e$[OIII] appears to be slightly higher for LISs. The much larger uncertainties associated with the T$_e$[OIII] of LISs do not allow robust conclusions. Moreover, the chemical abundances show no variation from one to another PN components, not even contrasting LISs with rims and shells, as also found in a number of other works. By discussing the ionization photon flux due to shocks and stellar radiation, we explore the possible mechanisms responsible for the excitation of LISs. We argue that the presence of shocks in LISs is not negligible, although there is a strong dependence on the orientation of the host PNe and LISs. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.10988v1
The survey of planetary nebulae in Andromeda M31 IV Radial oxygen and argon abundance gradients of the thin and thicker disc by Souradeep Bhattacharya et al. on Wednesday 21 September We obtain a magnitude-limited sample of Andromeda (M 31) disc PNe with chemical abundance estimated through the direct detection of the [OIII] 4363 $mathring{mathrm A}$ line. This leads to $205$ and $200$ PNe with oxygen and argon abundances respectively. We find that high- and low-extinction M 31 disc PNe have statistically distinct argon and oxygen abundance distributions. In the radial range $2-30$ kpc, the older low-extinction disc PNe are metal-poorer on average with a slightly positive radial oxygen abundance gradient ($0.006 pm 0.003$ dex/kpc) and slightly negative for argon ($-0.005 pm 0.003$ dex/kpc), while the younger high-extinction disc PNe are metal-richer on average with steeper radial abundance gradients for both oxygen ($-0.013 pm 0.006$ dex/kpc) and argon ($-0.018 pm 0.006$ dex/kpc), similar to the gradients computed for the M 31 HII regions. The M 31 disc abundance gradients are consistent with values computed from major merger simulations, with the majority of the low-extinction PNe being the older pre-merger disc stars in the thicker disc, and the majority of the high-extinction PNe being younger stars in the thin disc, formed during and after the merger event. The chemical abundance of the M 31 thicker disc has been radially homogenized because of the major merger. Accounting for disc scale-lengths, the positive radial oxygen abundance gradient of the M 31 thicker disc is in sharp contrast to the negative one of the MW thick disc. However, the thin discs of the MW and M 31 have remarkably similar negative oxygen abundance gradients. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2203.06428v2
NuSTAR observations of a heavily X-ray obscured AGN in the dwarf galaxy J144013+024744 by Shrey. Ansh et al. on Wednesday 21 September We present a multi-wavelength analysis of the dwarf Seyfert-2 galaxy J$144013+024744$, a candidate obscured active galactic nucleus (AGN) thought to be powered by an intermediate-mass black hole (IMBH, $M_bullet approx 10^{4-6} M_odot$) of mass $M_{bullet} sim 10^{5.2}M_odot$. To study its X-ray properties, we targeted J$144013+024744$ with NuSTAR for $approx 100$ ks. The X-ray spectrum was fitted with absorbed power law, Pexmon and a physical model (RXTorus). A Bayesian X-ray analysis was performed to estimate the posteriors. The phenomenological and the physical models suggest the AGN to be heavily obscured by a column density of $N_{rm H} = (3.4-7.0)times10^{23}$ cm$^{-2}$. In particular, the RXTorus model with a sub-solar metallicity suggests the obscuring column to be almost Compton-thick. We compared the $2-10$ keV intrinsic X-ray luminosity with the inferred X-ray luminosities based on empirical scaling relations for unobscured AGNs using $L_{rm [OIV](25.89mu {rm m})}$, $L_{[{rm OIII}](5007 {rm angstrom})}$, and $L_{6rm mu m}$ and found that the high-excitation $[{rm OIV}]$ line provides a better estimate of the intrinsic $2-10$ keV X-ray luminosity ($L_{2-10}^{rm int} sim 10^{41.41}{rm erg s}^{-1}$). Our results suggest that J$144013+024744$ is the first type-2 dwarf galaxy that shows X-ray spectroscopic evidence for obscuration. The column density that we estimated is among the highest measured to date for IMBH-powered AGNs, implying that a typical AGN torus geometry might extend to the low-mass end. This work has implications for constraining the black hole occupation fraction in dwarf galaxies using X-ray observations. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09913v1
CLASSY IV: Exploring UV diagnostics of the interstellar medium in local high- z analogs at the dawn of the JWST era by Matilde Mingozzi et al. on Wednesday 21 September The COS Legacy Archive Spectroscopic SurveY (CLASSY) HST/COS treasury program provides the first high-resolution spectral catalogue of 45 local high-z analogues in the UV (1200-2000AA) to investigate their stellar and gas properties. We present a toolkit of UV interstellar medium (ISM) diagnostics, analyzing the main emission lines of CLASSY spectra (i.e., NIV]$lambdalambda$1483,87, CIV$lambdalambda$1548,51, HeII$lambda$1640, OIII]$lambdalambda$1661,6, SiIII]$lambdalambda$1883,92, CIII]$lambdalambda$1907,9). Specifically, we focus our investigation on providing accurate diagnostics for reddening, electron density and temperature, gas-phase metallicity and ionization parameter, taking into account the different ionization zones of the ISM. We calibrate our UV toolkit using well-known optical diagnostics, analyzing archival optical spectra for all the CLASSY targets. We find that UV density diagnostics estimate ne values that are ~1-2 dex higher (e.g., ne(CIII]$lambdalambda$}1907,9)~10$^4$cm$^{-3}$) than those inferred from their optical counterparts (e.g., ne([SII]$lambdalambda$6717,31)~10$^2$cm$^{-3}$). Te derived from the hybrid ratio OIII]$lambda$1666/[OIII]$lambda$}5007 proves to be a reliable Te diagnostic, with differences in 12+log(O/H) within ~$pm$0.3dex. We also investigate the relation between the stellar and gas E(B-V), finding consistent values at high specific star formation rates, while at low sSFR we confirm an excess of dust attenuation in the gas. Finally, we investigate UV line ratios and equivalent widths to provide correlations with 12+log(O/H) and log(U), but note there are degeneracies between the two. With this suite of UV-based diagnostics, we illustrate the pivotal role CLASSY plays in understanding the chemical and physical properties of high-z systems that JWST can observe in the rest-frame UV. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09047v2
The survey of planetary nebulae in Andromeda M31 IV Radial oxygen and argon abundance gradients of the thin and thicker disc by Souradeep Bhattacharya et al. on Wednesday 21 September We obtain a magnitude-limited sample of Andromeda (M 31) disc PNe with chemical abundance estimated through the direct detection of the [OIII] 4363 $mathring{mathrm A}$ line. This leads to $205$ and $200$ PNe with oxygen and argon abundances respectively. We find that high- and low-extinction M 31 disc PNe have statistically distinct argon and oxygen abundance distributions. In the radial range $2-30$ kpc, the older low-extinction disc PNe are metal-poorer on average with a slightly positive radial oxygen abundance gradient ($0.006 pm 0.003$ dex/kpc) and slightly negative for argon ($-0.005 pm 0.003$ dex/kpc), while the younger high-extinction disc PNe are metal-richer on average with steeper radial abundance gradients for both oxygen ($-0.013 pm 0.006$ dex/kpc) and argon ($-0.018 pm 0.006$ dex/kpc), similar to the gradients computed for the M 31 HII regions. The M 31 disc abundance gradients are consistent with values computed from major merger simulations, with the majority of the low-extinction PNe being the older pre-merger disc stars in the thicker disc, and the majority of the high-extinction PNe being younger stars in the thin disc, formed during and after the merger event. The chemical abundance of the M 31 thicker disc has been radially homogenized because of the major merger. Accounting for disc scale-lengths, the positive radial oxygen abundance gradient of the M 31 thicker disc is in sharp contrast to the negative one of the MW thick disc. However, the thin discs of the MW and M 31 have remarkably similar negative oxygen abundance gradients. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2203.06428v2
CLASSY IV: Exploring UV diagnostics of the interstellar medium in local high- z analogs at the dawn of the JWST era by Matilde Mingozzi et al. on Tuesday 20 September The COS Legacy Archive Spectroscopic SurveY (CLASSY) HST/COS treasury program provides the first high-resolution spectral catalogue of 45 local high-z analogues in the UV (1200-2000{AA}) to investigate their stellar and gas properties. We present a toolkit of UV interstellar medium (ISM) diagnostics, analyzing the main emission lines of CLASSY spectra (i.e., NIV]{lambda}{lambda}1483,87, CIV{lambda}{lambda}1548,51, HeII{lambda}1640, OIII]{lambda}{lambda}1661,6, SiIII]{lambda}{lambda}1883,92, CIII]{lambda}{lambda}1907,9). Specifically, we focus our investigation on providing accurate diagnostics for reddening, electron density and temperature, gas-phase metallicity and ionization parameter, taking into account the different ionization zones of the ISM. We calibrate our UV toolkit using well-known optical diagnostics, analyzing archival optical spectra for all the CLASSY targets. We find that UV density diagnostics estimate ne values that are ~1-2 dex higher (e.g., ne(CIII]{lambda}{lambda}1907,9)~10^4cm^{-3}) than those inferred from their optical counterparts (e.g., ne([SII]{lambda}{lambda}6717,31)~10^2cm^{-3}). Te derived from the hybrid ratio OIII]{lambda}1666/[OIII]{lambda}5007 proves to be a reliable Te diagnostic, with differences in 12+log(O/H) within ~+/-0.3dex. We also investigate the relation between the stellar and gas E(B-V), finding consistent values at high specific star formation rates, while at low sSFR we confirm an excess of dust attenuation in the gas. Finally, we investigate UV line ratios and equivalent widths to provide correlations with 12+log(O/H) and log(U), but note there are degeneracies between the two. With this suite of UV-based diagnostics, we illustrate the pivotal role CLASSY plays in understanding the chemical and physical properties of high-z systems that JWST can observe in the rest-frame UV. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09047v1
Correcting for small-displacement interlopers in BAO analyses by Setareh Foroozan et al. on Tuesday 20 September Due to the low resolution of slitless spectroscopy, future surveys including those made possible by the Roman and Euclid space telescopes will be prone to line mis-identification, leading to interloper galaxies at the wrong redshifts in the large-scale structure catalogues. The most pernicious of these have a small displacement between true and false redshift such that the interloper positions are correlated with the target galaxies. We consider how to correct for such contaminants, focusing on $rm Hbeta$ interlopers in [OIII] catalogues as will be observed by Roman, which are misplaced by $Delta d = 97 ,h^{-1},{rm Mpc}$ at redshift $z = 1$. Because this displacement is close to the BAO scale, the peak in the interloper-target galaxy cross-correlation function at the displacement scale can change the shape of the BAO peak in the auto-correlation of the contaminated catalogue, and lead to incorrect cosmological measurements if not accounted for properly. We consider how to build a model for the monopole and quadrupole moments of the contaminated correlation function, including an additional free parameter for the fraction of interlopers. The key input to this model is the cross-correlation between the population of galaxies forming the interlopers and the main target sample. It will be important to either estimate this using calibration data or to use the contaminated small-scale auto-correlation function to model it, which may be possible if a number of requirements about the galaxy populations are met. We find that this method is successful in measuring the BAO dilation parameters without significant degradation in accuracy, provided the cross-correlation function is accurately known. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.05001v2
H1821+643: The most X-ray and infrared luminous AGN in the Swift BAT survey in the process of rapid stellar and supermassive black hole mass assembly by Hikaru Fukuchi et al. on Tuesday 20 September H1821+643 is the most X-ray luminous non-beamed AGN of $L_mathrm{14-150 keV}= 5.2times 10^{45}$ erg s$^{-1}$ in the Swift/BAT ultra-hard X-ray survey and it is also a hyper-luminous infrared (IR) galaxy $L_mathrm{IR} = 10^{13.2} L_odot$ residing in the center of a massive galaxy cluster, which is a unique environment achieving the rapid mass assembly of black holes (BH) and host galaxies in the local universe. We decompose the X-ray to IR spectral energy distribution (SED) into the AGN and starburst component using the SED fitting tool CIGALE-2022.0 and show that H1821+643 consumes a large amount of cold gas ($dot{M}_mathrm{con}$) with star-formation rate of $log ( mathrm{SFR}/M_{odot}~mathrm{yr}^{-1}) = 3.01 pm 0.04$ and BH accretion rate of $log (dot{M}_mathrm{BH}/M_{odot}~mathrm{yr}^{-1}) = 1.20 pm 0.05$. This high $dot{M}_mathrm{con}$ is larger than the cooling rate ($dot{M}_mathrm{cool}$) of the intra-cluster medium (ICM), $dot{M}_mathrm{con}/dot{M}_mathrm{cool} gtrsim 1$, which is one to two order magnitude higher than the typical value of other systems, indicating that H1821 provides the unique and extreme environment of rapid gas consumption. We also show that H1821+643 has an efficient cooling path achieving from $10^7$ K to $10^2$ K thanks to [OIII] 63 $mu mathrm{m}$, which is a main coolant in low temperature range ($10^4$ K to $10^2$ K) with a cooling rate of $dot{M}_{mathrm{cool}}=3.2times 10^5 M_{odot}mathrm{~yr^{-1}}$, and the star-forming region extends over 40 kpc scale. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09255v1
CLASSY IV: Exploring UV diagnostics of the interstellar medium in local high- z analogs at the dawn of the JWST era by Matilde Mingozzi et al. on Tuesday 20 September The COS Legacy Archive Spectroscopic SurveY (CLASSY) HST/COS treasury program provides the first high-resolution spectral catalogue of 45 local high-z analogues in the UV (1200-2000{AA}) to investigate their stellar and gas properties. We present a toolkit of UV interstellar medium (ISM) diagnostics, analyzing the main emission lines of CLASSY spectra (i.e., NIV]{lambda}{lambda}1483,87, CIV{lambda}{lambda}1548,51, HeII{lambda}1640, OIII]{lambda}{lambda}1661,6, SiIII]{lambda}{lambda}1883,92, CIII]{lambda}{lambda}1907,9). Specifically, we focus our investigation on providing accurate diagnostics for reddening, electron density and temperature, gas-phase metallicity and ionization parameter, taking into account the different ionization zones of the ISM. We calibrate our UV toolkit using well-known optical diagnostics, analyzing archival optical spectra for all the CLASSY targets. We find that UV density diagnostics estimate ne values that are ~1-2 dex higher (e.g., ne(CIII]{lambda}{lambda}1907,9)~10^4cm^{-3}) than those inferred from their optical counterparts (e.g., ne([SII]{lambda}{lambda}6717,31)~10^2cm^{-3}). Te derived from the hybrid ratio OIII]{lambda}1666/[OIII]{lambda}5007 proves to be a reliable Te diagnostic, with differences in 12+log(O/H) within ~+/-0.3dex. We also investigate the relation between the stellar and gas E(B-V), finding consistent values at high specific star formation rates, while at low sSFR we confirm an excess of dust attenuation in the gas. Finally, we investigate UV line ratios and equivalent widths to provide correlations with 12+log(O/H) and log(U), but note there are degeneracies between the two. With this suite of UV-based diagnostics, we illustrate the pivotal role CLASSY plays in understanding the chemical and physical properties of high-z systems that JWST can observe in the rest-frame UV. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09047v1
Correcting for small-displacement interlopers in BAO analyses by Setareh Foroozan et al. on Tuesday 20 September Due to the low resolution of slitless spectroscopy, future surveys including those made possible by the Roman and Euclid space telescopes will be prone to line mis-identification, leading to interloper galaxies at the wrong redshifts in the large-scale structure catalogues. The most pernicious of these have a small displacement between true and false redshift such that the interloper positions are correlated with the target galaxies. We consider how to correct for such contaminants, focusing on $rm Hbeta$ interlopers in [OIII] catalogues as will be observed by Roman, which are misplaced by $Delta d = 97 ,h^{-1},{rm Mpc}$ at redshift $z = 1$. Because this displacement is close to the BAO scale, the peak in the interloper-target galaxy cross-correlation function at the displacement scale can change the shape of the BAO peak in the auto-correlation of the contaminated catalogue, and lead to incorrect cosmological measurements if not accounted for properly. We consider how to build a model for the monopole and quadrupole moments of the contaminated correlation function, including an additional free parameter for the fraction of interlopers. The key input to this model is the cross-correlation between the population of galaxies forming the interlopers and the main target sample. It will be important to either estimate this using calibration data or to use the contaminated small-scale auto-correlation function to model it, which may be possible if a number of requirements about the galaxy populations are met. We find that this method is successful in measuring the BAO dilation parameters without significant degradation in accuracy, provided the cross-correlation function is accurately known. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.05001v2
O3 Mining Inc. is a gold exploration and development company focused on its assets located in Québec, Canada. The company forms part of the Osisko group of companies resulting in it benefitting from Osiko's expertise in successful mine development. The company's flagship properties include the Marban Project and the Alpha Project in the Val-d'Or district of Quebec. The Marban Project is located approximately 15 km west of the town of Val-d'Or and is a 1,023-hectare land package, consisting of approximately 30 mining claims and three mining concessions. The Alpha project of the company is a 7,754-hectare land package which is located 8 east of the town of Val-d'Or in Quebec, and 3 km south of the El Dorado South Lamaque Mine.
On the Origin of the Strong Optical Variability of Emission-line Galaxie by Ruqiu Lin et al. on Thursday 15 September Emission-line galaxies (ELGs) are crucial in understanding the formation and evolution of galaxies, while little is known about their variability. Here we report the study on the optical variability of a sample of ELGs selected in the COSMOS field, which has narrow-band observations in two epochs separated by $gtrsim$ 12 years. This sample was observed with Suprime-Cam (SC) and Hyper Suprime-Cam (HSC) on the $Subaru$ telescope in NB816 and $i'/i$ bands, respectively. After carefully removing the wing effect of a narrow-band filter, we check the optical variability in a sample of 181 spectroscopically confirmed ELGs. We find that 0 (0/68) Ha emitters, 11.9% (5/42) [OIII] emitters, and 0 (0/71) [OII] emitters show significant variability ($|Delta m_{NB}| geq 3,sigma_{Delta m_{NB,AGN}} = 0.20, mag$) in the two-epoch narrow-band observations. We investigate the presence of active galactic nucleus (AGN) in this variable ELG (var-ELG) sample with three methods, including X-ray luminosity, mid-infrared activity, and radio-excess. We find zero bright AGN in this var-ELG sample, but cannot rule out the contribution from faint AGN. We find that SNe could also dominate the variability of the var-ELG sample. The merger morphology shown in the HST/F814W images of all the var-ELG sample is in agreement with the enhancement of star formation, i.e., the SNe activity. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.07087v1
Empirical constraints on the turbulence in QSO host nebulae from velocity structure function measurements by Mandy C. Chen et al. on Monday 12 September We present the first empirical constraints on the turbulent velocity field of the diffuse circumgalactic medium around four luminous QSOs at $z!approx!0.5$--1.1. Spatially extended nebulae of $approx!50$--100 physical kpc in diameter centered on the QSOs are revealed in [OII]$lambdalambda,3727,3729$ and/or [OIII]$lambda,5008$ emission lines in integral field spectroscopic observations obtained using MUSE on the VLT. We measure the second- and third-order velocity structure functions (VSFs) over a range of scales, from $lesssim!5$ kpc to $approx!20$--50 kpc, to quantify the turbulent energy transfer between different scales in these nebulae. While no constraints on the energy injection and dissipation scales can be obtained from the current data, we show that robust constraints on the power-law slope of the VSFs can be determined after accounting for the effects of atmospheric seeing, spatial smoothing, and large-scale bulk flows. Out of the four QSO nebulae studied, one exhibits VSFs in spectacular agreement with the Kolmogorov law, expected for isotropic, homogeneous, and incompressible turbulent flows. The other three fields exhibit a shallower decline in the VSFs from large to small scales but with loose constraints, in part due to a limited dynamic range in the spatial scales in seeing-limited data. For the QSO nebula consistent with the Kolmogorov law, we determine a turbulence energy cascade rate of $approx!0.2$ cm$^{2}$ s$^{-3}$. We discuss the implication of the observed VSFs in the context of QSO feeding and feedback in the circumgalactic medium. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.04344v1
Empirical constraints on the turbulence in QSO host nebulae from velocity structure function measurements by Mandy C. Chen et al. on Monday 12 September We present the first empirical constraints on the turbulent velocity field of the diffuse circumgalactic medium around four luminous QSOs at $z!approx!0.5$--1.1. Spatially extended nebulae of $approx!50$--100 physical kpc in diameter centered on the QSOs are revealed in [OII]$lambdalambda,3727,3729$ and/or [OIII]$lambda,5008$ emission lines in integral field spectroscopic observations obtained using MUSE on the VLT. We measure the second- and third-order velocity structure functions (VSFs) over a range of scales, from $lesssim!5$ kpc to $approx!20$--50 kpc, to quantify the turbulent energy transfer between different scales in these nebulae. While no constraints on the energy injection and dissipation scales can be obtained from the current data, we show that robust constraints on the power-law slope of the VSFs can be determined after accounting for the effects of atmospheric seeing, spatial smoothing, and large-scale bulk flows. Out of the four QSO nebulae studied, one exhibits VSFs in spectacular agreement with the Kolmogorov law, expected for isotropic, homogeneous, and incompressible turbulent flows. The other three fields exhibit a shallower decline in the VSFs from large to small scales but with loose constraints, in part due to a limited dynamic range in the spatial scales in seeing-limited data. For the QSO nebula consistent with the Kolmogorov law, we determine a turbulence energy cascade rate of $approx!0.2$ cm$^{2}$ s$^{-3}$. We discuss the implication of the observed VSFs in the context of QSO feeding and feedback in the circumgalactic medium. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.04344v1
SFR estimations from z=0 to z=0 9 -- A comparison of SFR calibrators for star-forming galaxies by M. Figueira et al. on Monday 12 September Using VIPERS, we estimated a set of SFR based on photometric and spectroscopic data. We used, as estimators, photometric bands from ultraviolet to mid-infrared, and spectral lines. Assuming a reference SFR obtained from the spectral energy distribution reconstructed with Code Investigating GALaxy Emission, we estimated the reliability of each band as an SFR tracer. We used GSWLC to trace the dependence of these SFR calibrators with redshift. The far and near UV, u-band and 24-$mu$m bands, as well as $L_{TIR}$, are found to be good SFR tracers up to $zsim0.9$ with a strong dependence on the attenuation prescription used for the bluest bands (scatter of SFR of 0.26, 0.14, 0.15, 0.23, and 0.24dex for VIPERS, and 0.25, 0.24, 0.09, 0.12, and 0.12dex for GSWLC). The 8-$mu$m band provides only a rough estimate of the SFR as it depends on metallicity and polycyclic aromatic hydrocarbon properties (scatter of 0.23dex for VIPERS). We estimated the scatter of rest-frame luminosity estimations from CIGALE to be 0.26, 0.14, 0.12, 0.15, and 0.20dex for FUV, NUV, ugriz, K$_{mathrm{s}}$, and 8-24$mu$m-$L_{mathrm{TIR}}$). At intermediate redshift, the H$beta$ line is a reliable SFR tracer (scatter of 0.19dex) and the [OII] line gives an equally good estimation when the metallicity from the $R_{23}$ parameter is taken into account (0.17 for VIPERS and 0.20dex for GSWLC). A calibration based on [OIII] retrieves the SFR only when additional information such as the metallicity or the ionization parameter of galaxies are used (0.26 for VIPERS and 0.20dex for GSWLC), diminishing its usability as a direct SFR tracer. Based on rest-frame luminosities estimated with CIGALE, we propose our own set of calibrations from FUV, NUV, u-band, 8, 24$mu$m, $L_{TIR}$, H$beta$, [OII], and [OIII]. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.04390v1
SFR estimations from z=0 to z=0 9 -- A comparison of SFR calibrators for star-forming galaxies by M. Figueira et al. on Monday 12 September Using VIPERS, we estimated a set of SFR based on photometric and spectroscopic data. We used, as estimators, photometric bands from ultraviolet to mid-infrared, and spectral lines. Assuming a reference SFR obtained from the spectral energy distribution reconstructed with Code Investigating GALaxy Emission, we estimated the reliability of each band as an SFR tracer. We used GSWLC to trace the dependence of these SFR calibrators with redshift. The far and near UV, u-band and 24-$mu$m bands, as well as $L_{TIR}$, are found to be good SFR tracers up to $zsim0.9$ with a strong dependence on the attenuation prescription used for the bluest bands (scatter of SFR of 0.26, 0.14, 0.15, 0.23, and 0.24dex for VIPERS, and 0.25, 0.24, 0.09, 0.12, and 0.12dex for GSWLC). The 8-$mu$m band provides only a rough estimate of the SFR as it depends on metallicity and polycyclic aromatic hydrocarbon properties (scatter of 0.23dex for VIPERS). We estimated the scatter of rest-frame luminosity estimations from CIGALE to be 0.26, 0.14, 0.12, 0.15, and 0.20dex for FUV, NUV, ugriz, K$_{mathrm{s}}$, and 8-24$mu$m-$L_{mathrm{TIR}}$). At intermediate redshift, the H$beta$ line is a reliable SFR tracer (scatter of 0.19dex) and the [OII] line gives an equally good estimation when the metallicity from the $R_{23}$ parameter is taken into account (0.17 for VIPERS and 0.20dex for GSWLC). A calibration based on [OIII] retrieves the SFR only when additional information such as the metallicity or the ionization parameter of galaxies are used (0.26 for VIPERS and 0.20dex for GSWLC), diminishing its usability as a direct SFR tracer. Based on rest-frame luminosities estimated with CIGALE, we propose our own set of calibrations from FUV, NUV, u-band, 8, 24$mu$m, $L_{TIR}$, H$beta$, [OII], and [OIII]. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.04390v1
Metallicities of Five z > 5 Emission-Line Galaxies in SMACS 0723 Revealed by JWST by A. J. Taylor et al. on Monday 12 September JWST's Early Release Observations of the lensing cluster SMACS J0723.3-7327 have given an unprecedented spectroscopic look into the high-redshift universe. These observations reveal five galaxies at z > 5. All five have detectable [OIII]4363 line emission, indicating that these galaxies have high temperatures and low metallicities and that they are highly star forming. In recent work, the metallicities of these five galaxies have been studied using various techniques. Here we summarize and compare these previous results, as well as perform our own measurements of the metallicities using improved methodologies that optimize the extraction of the emission lines. In particular, we use simultaneous line fitting and a fixed Balmer decrement correction, as well as a novel footprint measurement of the emission lines in the 2D spectra, to produce higher fidelity line ratios that are less sensitive to calibration and systematic effects. We then compare our metallicities to those of z < 1 galaxies with high rest-frame equivalent widths of H-beta, finding that they may be good analogs. Finally, we estimate that the JWST galaxies out to z ~ 8 are young compared to the age of the universe. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.06418v2
Revisiting the Mass-Excitation MEx diagram using the MaNGA dataset by J. K. Barrera-Ballesteros et al. on Sunday 11 September The diagram comparing the flux ratio of the [OIII] and H$beta$ emission lines with the total stellar mass of galaxies (also known as the mass-excitation diagram, MEx) has been widely used to classify the ionization mechanism in high redshift galaxies between star formation and active galactic nuclear ones. This diagram was mainly derived using single-fiber spectroscopy from the SDSS-DR7 survey. In this study, we revise this diagram using the central and integrated spectral measurement from the entire Integral Field Spectroscopic MaNGA sample. Our results suggest that along with the physical parameters of this diagram, the equivalent width of the H$alpha$ emission line is also required to constrain the ionization mechanism of a high-redshifted galaxy. Furthermore, the location of a galaxy in the excitation-mass diagram varies depending on the use of central or integrated properties. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.03986v1
Metal-Enriched Neutral Gas Reservoir around a Strongly-lensed, Low-mass Galaxy at z=4 Identified by JWST NIRISS and VLT MUSE by Xiaojing Lin et al. on Thursday 08 September Direct observations of low-mass, low-metallicity galaxies at $zgtrsim4$ provide an indispensable opportunity for detailed inspection of the ionization radiation, gas flow, and metal enrichment in sources similar to those that reionized the Universe. Combining the James Webb Space Telescope (JWST), VLT/MUSE, and ALMA, we present detailed observations of a strongly lensed, low-mass ($approx 10^{7.6}$ ${rm M}_odot$) galaxy at $z=3.98$ (also see Vanzella et al. 2022). We identify strong narrow nebular emission, including CIV $lambdalambda1548,1550$, HeII $lambda1640$, OIII] $lambdalambda1661,1666$, [NeIII] $lambda3868$, [OII] $lambda3727$, and Balmer series of Hydrogen from this galaxy, indicating a metal-poor HII region ($lesssim 0.12 {rm Z}_odot$) powered by massive stars. Further, we detect a metal-enriched damped Ly$alpha$ system (DLA) associated with the galaxy with the HI column density of $N_{rm{HI}}approx 10^{21.8}$ cm$^{-2}$. The metallicity of the associated DLA may reach the super solar metallicity (${gtrsim Z}_odot$). Moreover, thanks to JWST and gravitational lensing, we present the resolved UV slope ($beta$) map at the spatial resolution of $approx 100$ pc at $z=4$, with steep UV slopes reaching $beta approx -2.5$ around three star-forming clumps. Combining with low-redshift analogs, our observations suggest that low-mass, low-metallicity galaxies, which dominate reionization, could be surrounded by a high covering fraction of the metal-enriched, neutral-gaseous clouds. This implies that the metal enrichment of low-mass galaxies is highly efficient, and further support that in low-mass galaxies, only a small fraction of ionizing radiation can escape through the interstellar or circumgalactic channels with low column-density neutral gas. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.03376v1
HI 21-cm absorption in radio-loud AGN with double-peaked OIII emission by Rajeshwari Dutta et al. on Wednesday 07 September Different physical processes in galaxy evolution, such as galaxy mergers that lead to coalescence of dual Active Galactic Nuclei (AGN) and outflows emanating from the narrow line region, can leave their imprint on the optical spectra of AGN in the form of double-peaked narrow emission lines. To investigate the neutral gas in the centres of such AGN, we have conducted a pilot survey of HI 21-cm absorption, using the upgraded Giant Metrewave Radio Telescope (uGMRT), in radio-loud AGN whose optical spectra show double-peaked [OIII] emission lines at z~50%) in the ground-based optical images than that for the systems that appear single and undisturbed (~25%). This is consistent with the high incidence of HI 21-cm absorption observed in z
Interview with Jose Vizquerra, President & CEO of O3 Mining Inc. (TSX-V:OIII) at THE Mining Investment Event of the North.
O3 Mining Inc. is a Canada-based mineral exploration company. The Company is focused on the acquisition, exploration, and development of precious metal resource properties in Canada and is primarily focused on Quebec. Its flagship properties include the Marban Property and the Alpha Property. The Company's 100% owned Marban Project is located approximately 15 kilometers west of the town of Val-d'Or in the Abitibi-Temiscamingue region of Quebec, Canada. It consists of approximately 30 mining claims and three mining concessions, covering approximately 1,023 hectares. The Alpha property is located eight kilometers east of Val-d'Or, Quebec, and three kilometers south of the El Dorado South Lamaque Mine. The property covers approximately 7,754 hectares and includes 20 kilometers of the prolific Cadillac Break. It also has additional projects in the Labrador and Abitibi areas of Quebec, which include Sleepy, Gwillim, Matachewan-Wydee, Harricana and other properties.
Oiii minha gente, muito feliz que chegou o dia de mais um devocional com vocês, sejam muito bem-vindas a esse cantinho
O3 Mining Inc. is a Canada-based mineral exploration company. The Company is focused on the acquisition, exploration, and development of precious metal resource properties in Canada and is primarily focused on Quebec. Its flagship properties include the Marban Property and the Alpha Property. The Company's 100% owned Marban Project is located approximately 15 kilometers west of the town of Val-d'Or in the Abitibi-Temiscamingue region of Quebec, Canada. It consists of approximately 30 mining claims and three mining concessions, covering approximately 1,023 hectares. The Alpha property is located eight kilometers east of Val-d'Or, Quebec, and three kilometers south of the El Dorado South Lamaque Mine. The property covers approximately 7,754 hectares and includes 20 kilometers of the prolific Cadillac Break. It also has additional projects in the Labrador and Abitibi areas of Quebec, which include Sleepy, Gwillim, Matachewan-Wydee, Harricana and other properties.
Oiii! Muito feliz de estar com você em mais um devocional juntas, e agora em um novo horário, bem cedinho, pro seu dia começar cheio de Deus
Oiii minha gente, vamos começar o dia tendo um tempo com Deus? E para o devocional de hoje vamos refletir em Efésios 2:8-9, onde Deus fala que somos salvos PELA GRAÇA por meio da fé, é o nosso Deus salvador
Oiii gente, bora pro devocional de hoje?
Oiii gente!! O caso de hoje no quadro LARI RESPONDE é sempre muuuito perguntado lá no meu Instagram (@larissaestradaa). Vamos falar sobre AMIZADE, e como é difícil ter boas amizades, né?! Se você também tem problemas com amizades, problemas com relacionamentos e sofre nessa área, então assiste o vídeo o final que vai te ajudar ♥
Oiii gente, mais um PODNOSSO no ar com a Kauane Leite e a Letícia Rivero
Oiii, viajaners! Hoje eu trouxe um casal incrível para contar histórias! A Gi e o João tem perrengues chiques, não … Mais
O3 Mining Inc is a Canada-based gold exploration company. The Company operates as a mine development and consolidator of exploration properties in gold camps in Canada. The Company holds a 100% interest in a number of properties in Quebec (137,000 hectares). The Company controls 61,000 hectares in Val D'Or and over 50 kilometers of strike length of the Cadillac-Larder Lake Faut. The Company also has a portfolio of assets in the James Bay and Chibougamau regions of Quebec. The Company's operated projects are Gwillim Property, The Cadillac Break Properties, Malartic Property and Alpha Property. The Cadillac Break Properties are located in the southeastern Abitibi Greenstone Belt of the Archean Superior Province in the Canadian Shield. The Gwillim property is located in the Barlow township, close to Chibougamau, consisting of 38 mining claims, covering 1715 hectares. It also owns the Denain-Pershing gold bearing property that covers approximately 10,001 hectares.
Oiii, viajaners! Neste episódio eu entrevistei essa pessoa incrível para conversar comigo e com vocês: a Ju Romano! o/ Além … Mais
O3 Mining Inc., an Osisko Group company, is a gold explorer and mine developer on the road to produce from its highly prospective gold camps in Québec, Canada. O3 Mining benefits from the support, previous mine-building success and expertise of the Osisko team as it grows towards being a gold producer with several multi-million ounce deposits in Québec.O3 Mining is well-capitalized and owns a 100% interest in all its properties (137,000 hectares) in Québec. O3 Mining trades on the TSX Venture Exchange (TSX.V: OIII) and on OTC Markets (OTCQX: OIIIF). The company is focused on delivering superior returns to its shareholders and long-term benefits to its stakeholders.
Oiii, viajaners! Neste episódio eu chamei meu amigo MARAVILHOSO Cleyton para contar dos maiores perrengues chiques da vida dele. Tem … Mais
Oiii, esse podcast tem o foco total na eterna rainha da sofrência Marilia Mendonça, nele nos falamos sobre sua trajetória, sua vida pessoal e principalmente o seu legado. Criado pelas alunas Maria Eduarda Fonseca, Marialyce Ingrid e Sabrina Cardoso da escola Ceep Professora Lourdinha Guerra. Espero que gostem!
Oiii, protagonistas! Gente, neste episódios existem algumas provocações para nos fazer refletir sobre o que somos capazes de fazer com o outro. Ah, se você gosta do meu conteúdo e do meu trabalho artístico saiba que o meu livro digital de poesias "A Estreia do Protagonista" está disponível na Amazon. Link: https://www.amazon.com.br/Estreia-do-Protagonista-Augusto-Haagensen-ebook/dp/B09M9DSKWD/ref=sr_1_3?__mk_pt_BR=%C3%85M%C3%85%C5%BD%C3%95%C3%91&keywords=a+estreia+do+protagonista&qid=1637852366&s=digital-text&sr=1-3
O3 Mining Inc., an Osisko Group company, is a gold explorer and mine developer on the road to produce from its highly prospective gold camps in Québec, Canada. O3 Mining benefits from the support, previous mine-building success and expertise of the Osisko team as it grows towards being a gold producer with several multi-million ounce deposits in Québec.O3 Mining is well-capitalized and owns a 100% interest in all its properties (137,000 hectares) in Québec. O3 Mining trades on the TSX Venture Exchange (TSX.V: OIII) and on OTC Markets (OTCQX: OIIIF). The company is focused on delivering superior returns to its shareholders and long-term benefits to its stakeholders.
O3 Mining Inc is a Canada-based gold exploration company. The Company operates as a mine development and consolidator of exploration properties in gold camps in Canada. The Company holds a 100% interest in a number of properties in Quebec (137,000 hectares). The Company controls 61,000 hectares in Val D'Or and over 50 kilometers of strike length of the Cadillac-Larder Lake Faut. The Company also has a portfolio of assets in the James Bay and Chibougamau regions of Quebec. The Company's operated projects are Gwillim Property, The Cadillac Break Properties, Malartic Property and Alpha Property. The Cadillac Break Properties are located in the southeastern Abitibi Greenstone Belt of the Archean Superior Province in the Canadian Shield. The Gwillim property is located in the Barlow township, close to Chibougamau, consisting of 38 mining claims, covering 1715 hectares. It also owns the Denain-Pershing gold bearing property that covers approximately 10,001 hectares.
Oiii gente, tudo bom? Esse é o último episódio do nosso mês especial, com episódios todos os dias aqui no podcast. Quero muito agradecer por terem ouvido, compartilhado nosso conteúdo e espero que vocês tenham gostado do Complicando o Simplificando
Oiii hoje eu vou fazer um tutorial de como eu arrumo minha mala e também irei dar algumas dicas.
O3 Mining Inc., an Osisko Group company, and is a gold explorer and mine developer ready to produce from its highly prospective gold camps in Québec, Canada. O3 Mining benefits from the support, previous mine-building success and expertise of the Osisko team as it grows towards being a gold producer with several multi-million ounce deposits in Québec.The company has 2 very important projects in Quebec, Marban and Alpha. There is over 3.9Moz at the Val D'Or property, one of the best mining areas in the world. O3 is currently moving the Marban project towards production in 2026 and there is a lot of exploration potential which could increase the amount of resources for the company and increase the value for shareholders.O3 is well funded and the company is being very systematic with the development of the Marben resource. Now that they have reached a 2.5Moz resource at Marban, they are focused on moving ahead towards production. They plan to invest $256M in capex, they have completed the PEA and are in the process of working towards the PFS now and then onto the Feasibility Study for the project.As Marban moves towards production, O3 will continue to drill to continue to improve and modify the engineering of the project and this will increase the size and value of the resource. O3 has a systematic approach to looking for further discoveries and is drilling on the western side of Marban and also in 4 different areas at Alpha. They hope to execute the project at Marban to produce cash flow and at the same time add to the resource at Alpha with potentially a much bigger discovery in the future. O3 Mining owns a 100% interest in all its properties (137,000 hectares) in Québec. O3 Mining trades on the TSX Venture Exchange (TSX.V: OIII) and on OTC Markets (OTCQX: OIIIF). The company is focused on delivering superior returns to its shareholders and long-term benefits to its stakeholders.
The fellas talk about Luffy's skating abilities and Nami's meta gaming tactics. @PandaSightings PandaSightings@gmail.com for questions Intro song was "Oiii!" from the Cursed Sword OstThank you for showing up to our annual hotdog eating contest.Spongebob memes will forever be humanity's greatest creation~
Finalmente, voltei. (Eu juro que não abandonei vocês, inclusive, em breve teremos novidades) Oiii, viajaners! Neste episódio eu trouxe para … Mais
Oiii amigos, o jogo da discórdia foi tudo, mais uma vez admiro a coragem do João em escancarar o racismo que ele sofreu levantando essa pauta super importante! --- Support this podcast: https://anchor.fm/nada-de-metades/support
Oiii gentem!!!E chega ao fim a segunda temporada de Soltos em Floripa, chegamos aqui até aqui com uma jornada divertida e perceptível a evolução dos solteiros! Nos vemos na próxima!!! --- Support this podcast: https://anchor.fm/nada-de-metades/support
Oiii!!! coom un down 'nd 'ave a coople pints laddie!!! 'ave aa coople laughs!!! Mad Mac, Professor Satan, and special guest Zackajawea sit down and talk about a bunch of shite while celebrating Saint Patrick's Day. ******DO NOT TAKE WHAT WE SAY TO HEART THEY ARE JOKES!!!******* NOW ENJOY THE SHOW!!!! --- Support this podcast: https://podcasters.spotify.com/pod/show/outsidethecircle23/support
Oiii amigos, no episódio de hoje eu trago convidados muito mais que especiais que eu conheci no meu primeiro voluntáriado no Recanto de Ode, falamos sobre essa experiência e vivência única!! Thank you girls to do this with me, and Lucas valeu pela força e alegria de sempre!!! Always in my heart ❤ --- Support this podcast: https://anchor.fm/nada-de-metades/support
Oiii aqui é Dudinha, sou amiguinha da Aline... E eu vim aqui para cantar pra vocês
Interview with Jose Vizquerra, President & CEO of O3 Mining (TSX-V:OIII)
Oiii amigos e não é que esse BBB tá sendo Plot Twist atrás de Plot Twist. No episódio de hoje eu falo um pouco do que achávamos na primeira semana e como tudo mudou, liderança de João e um dos melhores memes do BBB21 até agora! --- Support this podcast: https://anchor.fm/nada-de-metades/support
Oiii, viajaners! No episódio de hoje eu trouxe a produtora de TV Renata Motta para contar suas experiências incríveis com … Mais
Oiii, viajaners! Hoje eu estou super bem acompanhada pela talentosíssima Juliana Munaro. Essa jornalista maravilhosa me deu a honra de … Mais
Oiii, viajaners! Olha só quem é a convidada deste episódio: a Ira Croft, lá do Programa Ponto G e Mundo Freak! A rainha da … Mais
Oiii galerinha do bem, tudo na paz por aí? No episódio de hoje, vamos analisar as fontes... lembrando que fonte, além de estar associada a água, no seu sentido mais puro, também está relacionada a origem, princípio, fundamento. E nos dois sentidos, vamos analisar algumas fontes que sobrecarregam o nosso coração . Espero que essa análise possa fazer vc repensar e melhorar isso na sua vida. Vem comigo pra entender melhor. Bjo no coração e fiquem com Deus. --- Send in a voice message: https://anchor.fm/pamicast/message
OIII, TUDO BEM? olha quem resolveu aparecer novamente... EU! E não é que rolou play mesmo. UAU! E a Pandemia... um D E S A B A F O! E como você está? aconteceu algo estranho durante seu confinamento?
Oiii... Guys, ini gw bakalan ngasih tau beberapa jajanan tradisional yg enak tapi sayangnya udah hampir terlupakan di zaman sekarang. Check it out !
Oiii, gente, chegamos ao nosso penúltimo eps sobre o livro da Bell Hooks, Teoria feminista: da margem ao centro. No eps de hoje, falaremos sobre o cap 7, 8 e 9. O títulos dos caps são: 7 Repensando a natureza do trabalho 8 Educando mulheres uma agenda feminista / 9 O movimento feminista para acabar com a violência, espero que gostem. BOM EPISÓDIOOO !
Parece, mas internet não é terra de ninguém.No EP12 as Tikalakatikas contam o que consideram o limite do aceitável no quesito traições online, falam sobre dividir a senha do celular com o boy, descobrir uma troca de mensagens entre ele e uma ex-peguets, encontrar o perfil do namorado da miga no Tinder, deletar rastros no Whatsapp, não perdoar nem um “Oiii” com 3 “is” e várias outras psicopatias.Pra seguir no Instagram: Tikalakatika Podcast - @tikalakatikapodcast • Camile Liguori - @camile_liguoriLarissa Avelino - @laavelinor Vanessa Cristina - @vanbanana3 • Mande um salve: tikalakatikapodcast@gmail.com•Ouça também pelo:Spotify - http://bit.ly/TikasNoSpotifyEP12Apple Podcasts - http://bit.ly/TikasNoApplePodcastsEP12Youtube - http://bit.ly/TikasNoYoutubeEP12 Spreaker - http://bit.ly/TikalakatikaEP12 --- Send in a voice message: https://anchor.fm/tikalakatikapodcast/message
Fakultät für Physik - Digitale Hochschulschriften der LMU - Teil 05/05
The work presented in this thesis studies the role that accretion events play in the evolution of galaxies in dense environments, such as galaxy clusters. Cosmological simulations allow us to study in detail the evolution of galaxies' halos in cluster environments and have shown that the formation of extended halos around central cluster galaxies and intracluster light (ICL) is closely correlated to the morphological transformation of galaxies in clusters. However, the extremely low surface brightness of these components makes it difficult to gather observational constraints. This thesis studies the light and stellar motion in the halo of the giant elliptical galaxy M87 and its surrounding IC component at the centre of the Virgo cluster. Virgo is the nearest ($sim 15$~Mpc away) large scale structure, a young cluster characterised by both spatial and kinematic substructures. M87 has one of the oldest stellar populations in the local Universe and a stellar halo that contains $sim$ 70% of the galaxy light down to $rm{mu_{V}=27, mag, arcsec^{-2}}$. Moreover, deep images of the Virgo cluster core have revealed an extended network of tidal features suggesting that accretion events characterise its mass assembly. Thus, M87 and its host environment are prime targets to shed light on the hierarchical assembly of structure in the Universe. This work uses new Suprime-Cam@Subaru photometry and FLAMES@VLT spectroscopy to study a $sim 0.5, rm{deg^2}$ area around M87, in the transition region between galaxy halo and ICL. We use planetary nebulas (PNs) as tracers, whose strong [OIII] $lambda$5007 AA emission line makes them excellent photometric and kinematic probes, also at large distances from the galaxy's centre. The photometric analysis of the PN sample shows the superposition of two stellar populations, both halo and ICL. This is confirmed by spectroscopically detected PNs, whose velocity phase-space also reveals that halo and ICL split into two different kinematic components. They have very different spatial distributions and parent stars, as indicated by the properties of the PN populations they are associated with, such as the $alpha$-parameter and the slope of the planetary nebula luminosity function (PNLF). In this thesis I give the observational proof that in Virgo the central galaxy and the ICL both evolve through the ongoing accretion of smaller systems. However, stellar halo and ICL are dynamically distinct components with different velocity and density distributions, and parent stellar populations. Whether or not these conclusions are true for different galaxies in different Virgo subclusters is still an open question and the topic of one of my planned future studies.
Fakultät für Physik - Digitale Hochschulschriften der LMU - Teil 04/05
This work aims at enabling quantitative optical nitrogen line spectroscopy in O-stars, in order to improve our knowledge about these objects, particularly their earliest spectral subtypes. To this end, nitrogen has proven to be a key element, both in terms of its potential to infer effective temperatures, and for being the best tracer for testing the effects of rotational mixing in massive stellar models, allowing us to further constrain the evolution of massive stars. To accomplish this study, we used the NLTE (non local thermodynamic equilibrium) atmosphere/spectrum synthesis code FASTWIND, and developed a new nitrogen model atom, partly based on older work, comprising the ionization stages NII to NV. Moreover, we incorporated the dielectronic recombination mechanism into FASTWIND, which was previously unable to deal with this process. We performed an extensive investigation on the line-formation process of strategic nitrogen emission lines such as NIII4640 and NIV4058, accounting for a complete treatment of line blocking/blanketing effects and the presence of a wind, as it is possible when using a state-of-the-art atmospheric code. Contrasted to the results from the seminal work on the NIII triplet formation performed by Mihalas & Hummer (1973), based on much simpler model atmospheres, our study implies that dielectronic recombination plays only a secondary role under Galactic conditions. Rather, the emission is controlled by the stellar wind (Swings mechanism), as long as the wind is powerful enough to enable a significantly accelerating velocity field already in the photospheric formation region. For later spectral O-subtypes, the strength of the emission might be also affected by an OIII resonance line overlapping with the NIII resonance line in the EUV. Concerning the emission at NIV4058, we suggest a rather similar mechanism. Also in this case, the dominating process is the strong depopulation of the lower level of the transition, which increases as a function of the wind-strength. Unlike the NIII triplet emission, however, resonance lines do not play a role for typical mass-loss rates and below. Using the updated version of FASTWIND and our new model atom, we derived nitrogen abundances for a substantial O-star sample in the Large Magellanic Cloud (LMC). Stellar and wind parameters of our sample stars were determined by line profile fitting of hydrogen, helium and nitrogen lines, exploiting the corresponding ionization equilibria. The bulk of our sample stars turned out to be strongly nitrogen-enriched, and a clear correlation of nitrogen and helium enrichment was found. By comparing the nitrogen abundances as a function of projected rotation velocity with tailored evolutionary calculations, we identified a considerable number of highly enriched, but slowly rotating object, which should not exist according to standard theory of rotational mixing. Our findings support the basic outcome of previous B-star studies within the VLT-FLAMES survey on massive stars which pointed to similar discrepancies. The detection of strong nitrogen enrichment in the bulk of our sample stars indicates that efficient mixing takes place already during the very early phases of stellar evolution of LMC O-stars. In the last part of this thesis, we concentrated on the applicability of the Walborn et al. (2002) classification scheme for very early O-stars, which is primarily based on the relative strengths of the NIV4058 and NIII4640 emission lines. This scheme has already been used in a variety of studies, but is still disputed for various reasons. We provided first theoretical predictions on the NIV4058/NIII4640 emission line ratio in dependence of different parameters, and confronted these predictions with results from an analysis of a sample of early-type LMC/SMC O-stars. Though we found a monotonic relationship between the NIV/NIII emission line ratio and the effective temperature, all other parameters being equal, our predictions indicate additional dependencies on other important stellar parameters, most significantly, the nitrogen abundance. The relation between the observed NIV/NIII emission line ratio and the effective temperature, for a given luminosity class, turned out to be quite monotonic for our sample stars, and to be fairly consistent with our model predictions. The scatter within a spectral subtype is mainly produced by abundance effects. Our findings suggest that the Walborn et al. classification scheme is able to provide a meaningful relation between spectral type and effective temperature, as long as it is possible to discriminate for the luminosity class.
Lalalalala * música dos happy tree friends* Oiii, semana passada me seqüestraram e eu não pude postar o PodCast, mas isso não vai acontecer de novo *pega a bazuca* e pra quem não conhece eu sou a Raid. Dando segmento a corrida dos chibi cast’s um especial de música japa. Sky, Mugi, Kuroki, Marcos e … O post AFS – 039 – J-list : 2009/2010, Opens de Animes apareceu primeiro em Anime Freak Show v7.0.
Fakultät für Physik - Digitale Hochschulschriften der LMU - Teil 02/05
Several lines of evidence suggest that the most active phase of galaxy evolution, especially in the most massive systems, was largely completed by $zsim 1$. This results, e.g., from the observation that the most massive galaxies at low redshift have very old stellar populations ($sim 10$ Gyr) and very little gas to fuel subsequent star formation. Similarly, active galactic nuclei (AGN) were more numerous and brighter in the early universe. Ultimately, the direct observation of high-redshift galaxies will be the only way to understand which processes shaped the universe we see today, in spite of the rich ``fossil'' data sets we have of the Milky Way and neighboring galaxies. Thanks to the new $8-10$ m telescope class and novel instrumentation, including SPIFFI/SINFONI on the VLT, individual galaxies at redshifts $zsim 1-3$ ($2-6$ Gyr after the Big Bang) are now within the reach of astronomical spectrographs. Methodologically, this thesis focuses on the analysis of spectrally and spatially resolved optical emission lines, first of all ha and [OIII]lam5007, which are shifted into the near-infrared. {sc Spiffi / Sinfoni} is very suited to such a programme, because it records the spectra of a contiguous field of view of up to 8arcsec$times$8arcsec. The internal kinematic and chemical gradients within a galaxy can thus be measured in a single observation. Galaxies in the early universe had particularly high star-formation rates, so that many targets are bright optical line emitters. Internal kinematics are measured through the Doppler effect, line profiles and widths indicate the presence of an AGN, galactic ``superwinds'' and the relationship of chaotic to ordered motion. Star-formation rates are measured from the luminosity of the Balmer lines, especially ha. Characteristic line ratios indicate the presence of an AGN, chemical composition, and electron densities in the ISM, and they allow to distinguish shocks and photoionization. This thesis is a pilot study: It comprises 9 galaxies that fulfill a variety of selection criteria: they are either bright UV or submillimeter emitters, or they are radio-loud. Perhaps the most fundamental result is that gravity (dominated by dark matter) is the main driver of early galaxy evolution, but it is not the only important process. Star formation and AGN cause hydrodynamical feedback processes, which might be a sign of self-regulated galaxy evolution. It is found that star-formation related feedback had similar properties at low and high redshift, but that AGN-driven gas expulsion might have played a major role in the high-redshift evolution of galaxies, that is without low-redshift equivalent. Another important result is the rotation curve we find in the central kiloparsec of a gravitationally lensed UV-selected galaxy. Velocity gradients of $sim 100$ kms have been observed in many high-redshift galaxies, but the interpretation as rotation curves is generally not unique. Given the relatively coarse spatial resolution of high-redshift galaxy data, two nearby galaxies, maybe interacting or undergoing a merger, might blend into one smooth velocity gradient. Galaxy mergers are an important ingredient of the ``hierarchical model'', the current paradigm of structure formation, and therefore nearby galaxy pairs were likely more common at high redshift than they are today. The large similarity of the lensed rotation curve with those of nearby galaxies might be a first sign that galaxies evolved inside-out.