Recent Results of the MPE Infrared/Submillimeter Group
A spatially resolved quasar broad line region
Knowing the structure, size, and dynamics of the Broad Line Regions (BLRs) near accreting supermassive black holes would allow to constrain the inward and outward transport mechanisms and to infer the mass of the black hole. So far, however, directly measuring BLR properties was impossible because of its small physical size, on the order of hundreds of light-days (corresponding to an angular size <1mas). With GRAVITY we have now, for the first time, spatially resolved (10 micro-arcseconds or ~0.03 parsec for a distance of 550 mega-parsecs) a velocity gradient across the broad line region of the quasar 3C 273. The gradient reveals rotation perpendicular to the jet, and is consistent with line emission from a thick disc of gravitationally bound material around a black hole of 3 x 108 M. We infer a disc radius of 150 light-days (compared to 100-400 light-days found previously from Reverberation Mapping - RM). Thus, GRAVITY provides both a confirmation of RM (at least for this one object) as the main previous method to determine black hole masses in quasars and a new and highly accurate, independent method to measure such masses. In an approved VLTI Large Program we will extend this study to a (small) sample of local AGN, and we are exploring options to expand it to larger samples and higher redshifts with potential upgrades of GRAVITY.
- MPE News http://www.mpe.mpg.de/6966658/news20181129
- Research paper: GRAVITY Collaboration: Sturm, E., Dexter, J. et al. 2018, Nature, Vol. 563, p.657
Outflow demographics and physical properties at z ~ 1 – 3
Exploiting our full KMOS3D and SINS/zC-SINF surveys of near-IR IFU spectroscopy of z~1–3 galaxies, we obtained the most complete census to date of galactic-scale ionized gas outflows at the peak epoch of cosmic star formation and AGN activity. The sample of ~600 primarily mass-selected galaxies spans wide ranges in stellar mass and star formation rate; the selection by mass, rather than by properties biased towards star formation (SF) or AGN activity, makes it ideally suited for a population-averaged characterization of winds as relevant to galaxy evolution. Compared to slit spectra, the IFU data greatly facilitates the separation between the broad outflow component in Ha+[NII]+[SII] and the narrower component from star formation. Our studies show how outflows driven by SF and by AGN are spatially, spectrally, and demographically distinct. SF-driven winds, launched near bright star-forming clumps across disks, have typical speeds ~450 km/s below the hosts’ escape velocity except at log(MÛ/M) 10.3; the prevalence of these winds depends on SF properties, not mass. AGN-driven winds originate from the nuclear regions, are ubiquitous in log(MÛ/M) 10.7 galaxies hosting a massive bulge but rare at lower masses, irrespective of SF activity; with velocities of ~1500 km/s, they can escape the galaxies. The high S/N spectra constrain for the first time the density in high-z SF-driven winds from the broad [SII] doublet ratio, yielding ne ~ 400 cm–3; for AGN-driven winds, a higher ne~1000 cm–3 is inferred. These densities are a factor of several higher than previously assumed values, and lead to correspondingly more modest mass outflow rates ~0.1–0.4´SFRs in warm ionized gas. The tension with theoretical work, requiring mass outflow rates SFRs to reproduce the observed galaxy mass–metallicity and galaxy mass – halo mass relationships at log(MÛ/M)<10.7, could be alleviated if substantial mass, momentum, and energy are ejected in hotter and/or colder phases than the ~104 K ionized gas probed by our data. The fast, high duty cycle AGN-driven winds at high masses carry significant energy (~1% that of the AGN), which may contribute to heat halo gas and help prevent further gas infall. Our results are consistent with recent EAGLE and Illustris/TNG numerical simulations, which suggest that such a mechanism, acting also at the modest luminosities and Eddington ratios of the majority of the KMOS3D and SINS/zC-SINF AGN, may be more effective at widespread and long-term quenching than ejective “QSO mode” feedback in rare, high luminosity, high Eddington ratio AGN.
Scaling relations for molecular gas in Galaxies over cosmic time
We have developed new statistically robust scaling relations between galaxy integrated molecular gas masses, stellar masses and star formation rates (SFR) relative to that on the main sequence (δMS). Combining data from our PHIBSS and xCOLDGASS surveys with data from the literature, we use three independent methods to determine molecular gas masses: 1) CO line fluxes, 2) Herschel far-infrared dust SEDs, and 3) ~1mm dust photometry, in a large sample of 1444 star forming galaxies and stacks between z=0 and 4. The sample spans stellar masses from log(M*/M8)=9.0-11.8, and star formation rates relative to that on the MS, from 10-1.3 to 102.2. The most important result is that all data sets follow the same scaling trends, once we consistently account for uncertainties and apply consistent methodologies. The molecular gas depletion time tdepl, defined molecular gas mass/star formation rate, scales as (1+z)-0.6 ´ (δMS)-0.44, and is only weakly dependent on stellar mass. The ratio of molecular-to-stellar mass μgas depends on (1+z)2.5´ (δMS)0.52´ (M*)-0.36, and tracks the evolution of the specific star formation rate.
Strongly baryon-dominated disk galaxies at the peak epoch of galaxy formation.
New observations of rotating galaxies at z~2, the peak epoch of galaxy formation, show that these massive star-forming galaxies are strongly dominated by baryonic mass, with dark matter playing a much smaller role in comparable regions of their outer disks than in typical present-day spiral galaxies. This result was obtained from observations of unprecedented sensitivity with the SINFONI and KMOS near-IR integral field spectrometers, mapping the 2D kinematics of ionized gas through the Halpha line emission of six galaxies out to 2-3 times their half-light radius. On these scales, dark matter starts to dominate the total mass budget in z~0 late-type galaxies, causing their rotation curves to stay mostly flat or to slightly increase with radius. In contrast, the six individual massive z~2 galaxies in our study exhibit declining rotation curves, which can be explained by the combination of two factors: baryons dominate more strongly than dark matter on galactic scales, and the elevated gas turbulence characteristic of z~2 disks provides a significant amount of the dynamical support -- thereby leading to a decrease in the rotation velocity. Such a falloff with radius is further seen in the average outer rotation curve derived through a novel stacking technique of ~100 typical massive z~1-2.5 disk galaxies observed with KMOS and SINFONI, suggesting that it is a common feature among the star-forming population at these epochs. Two additional studies of the resolved inner disk kinematics (out to 1-1.5 half-light radius or the velocity turnover radius) of 240 star-forming disks support the results based on the outer rotation curves. Detailed dynamical modeling shows that while the stars+gas account on average for ~56% of the total enclosed mass at z~1-2.5, the baryon fraction reaches ~90% at the higher redshifts, and is largest in disks with highest central baryonic mass surface density. The evolution of the zero-point stellar and baryonic Tully-Fisher relationships based on the same data is further compatible with the increase in gas and baryon mass fractions with redshift, with a lesser role of dark matter in the central disk regions. The low galactic-scale dark matter fractions found in massive high-redshift galaxies in these studies are comparable to those of present-day massive early-type galaxies, their likely descendants. The high gas fractions in z~2 star-forming galaxies could help to dissipate angular momentum, efficiently driving gas inwards and leading to the strong dominance of baryons early on.
- Genzel et al. 2017, Nature, 543, 397
- Lang et al. 2017, ApJ, 840, 92
- Übler et al. 2017, ApJ, 842, 121
- Wuyts et al. 2016, ApJ, 831, 149
KMOS3D survey of spatially-resolved gas kinematics, star formation, and ISM properties sheds new light on the physics of galaxy evolution
Our comprehensive and highly successful multi-year KMOS3D survey takes advantage of the efficient multiplexing of the new near-IR 24-IFU KMOS instrument at the Very Large Telescope to spatially resolve the ionized gas kinematics, star formation, outflows, excitation, and metallicities of a large and homogeneous sample of z ~ 0.7 − 2.7 mass-selected galaxies. KMOS3D is a 75-night Garanteed Time Program begun in November 2013 and led jointly by the MPE IR/Submm group and MPE/OPINAS+USM. After 2.5 years and 52 nights of productive observing campaigns, the sample has now reached 564 galaxies, with an overall Hα detection fraction of 80% (and as high as 90% for main-sequence star-forming galaxies). The survey is carried out in well-studied extragalactic fields, benefitting from extensive multi-wavelength data that include the far-IR Herschel PEP survey and high-resolution near-IR/optical grism and imaging data from the 3D-HST/CANDELS HST Treasury programs. KMOS3D is designed to provide an unbiased census from deep integrations (~ 5h − 25h) of the Hα+[NII]+[SII] line emission resolved on seeing-limited scales of 4 − 5 kpc, over a wide range of galaxy parameters and 5 billion years of cosmic time. The strategy is uniquely enabling faint line emission mapping in individual objects and pushing near-IR IFU studies into new regimes such as lower mass star-forming galaxies, and high-mass sub-main sequence galaxies in the process of quenching. Our results, with highlights shown in the Figure, now 1) robustly confirm the earlier findings from our SINS/zC-SINF near-IR IFU survey with SINFONI on the majority of disks among high-z star-forming galaxies and their elevated gas turbulence compared to present-day spirals, and on the ubiquity and origin of powerful AGN- and star formation-driven gas outflows, 2) provide new constraints on the angular momenta, baryonic mass fractions, outer disk structure, mass-metallicity-star formation relation, and gas-phase O/H abundance gradients, and 3) shed new light on dense core formation and star formation quenching in high-mass galaxies.
- Wisnioski et al. 2015, ApJ, 799, 209
- Burkert et al. 2016, ApJ, 826, 214
- Wuyts, S. et al. 2016, ApJ, 831, 149
- Wuyts, E. et al. 2016, ApJ, 827, 74
ALMA reveals planetary construction sites
Using the Atacama Large Millimeter/submillimeter Array (ALMA), the clearest indications yet have been found that planets with masses several times that of Jupiter have recently formed in the discs around young stars. New images of transitional discs show that there are significant amounts of gas within the dust gaps, and that the gas also possessed a gap, up to three times smaller than that of the dust. This can only be explained by the scenario in which newly formed massive planets have cleared the gas as they travelled around their orbits, but trapped the dust particles further out. The data rule out other scenarios for the observed set of discs.
Evidence for widespread AGN-driven outflows in the most massive z~1-2 star-forming galaxies
Very deep laser guide star assisted adaptive optics observations have allowed us to detect ubiquitous powerful nuclear outflows in massive (1011 MSun) z ∼ 2 star-forming galaxies, which are plausibly driven by an active galactic nucleus (AGN). The spectra in their central regions exhibit a broad component in Hα and forbidden [N II] and [S II] line emission, with typical velocity FWHM ∼ 1500 km s-1, high [NII]/Hα ratio ≈ 0.6, and intrinsic extent of 2–3 kpc. At larger radii, weaker and less wide broad components suggest star formation driven outflows. The high inferred nuclear mass outflow rates and frequent occurrence suggest that the nuclear outflows efficiently expel gas out of the centers of the galaxies with high duty cycles and may thus contribute to the process of star formation quenching in massive galaxies. Extending to a large sample observed without adaptive optics, we find that the incidence of the most massive galaxies with broad nuclear components is at least as large as that of AGNs identified by X-ray, optical, infrared, or radio indicators, as expected for rapidly varying AGN whose outflows are visible with larger duty cycle than X-ray or optical continuum. The mass loading of the nuclear outflows is near unity. Our findings provide compelling evidence for powerful, high-duty cycle, AGN-driven outflows near the Schechter mass, and acting across the peak of cosmic galaxy formation.
- Research paper: Förster Schreiber et al. 2014 ApJ 787, 38
- Research paper: Genzel et al. 2014 ApJ 796, 7
Molecular gas, extinction, star formation and kinematics in the z=1.5 star forming galaxy EGS130111661
As a follow-up to the high-redshift molecular gas survey PHIBBS (Tacconi et al. 2013; see news item below), a detailed study was performed of one of the most massive galaxies in this survey. For the study of the galaxy named EGS13011166, CO 3-2 line observations from the IRAM Plateau de Bure millimeter interferometer were combined with Large Binocular Telescope (LBT) LUCI observations of the H-alpha line in this galaxy, at matched spatial resolutions of 0.75 arcseconds. The galaxy was scanned perpendicular to the slit with LUCI to obtain spatially resolved spectra both along and perpendicular to the slit. Additionally, Hubble Space Telescope (HST) V-I-J-H band maps were used. Together these data allow to derive the stellar surface density and star formation rate, molecular gas surface density, optical extinction and gas kinematics.
- Research paper: Genzel et al. 2013, The Astrophysical Journal 778, 68
New observations on the Galactic Center gas cloud "G2"
September 12, 2012
New observations on the gas cloud "G2" falling towards the Galactic Center confirm its highly elliptical orbit, but with updated orbital parameters. With the new data, the cloud is now expected to come even closer -- the updated pericenter distance is 2200 Schwarzschild radii -- to the super-massive black hole at the center of our galaxy. While its origin is still unclear, its apocenter is near the inner edge of the disk of young stars. This supports speculations that the cloud, which has a mass of only about three earth masses, originated as a wind of one of these stars.
In the course of this year, more observations of the cloud are planned, of course, and not only in the infrared but campaigns have been started by many groups to observe this accretion event in the whole electromagnetic spectrum. A wiki page has been set up to collect all information on "G2".
Galactic Black Hole disrupts Gas Cloud
December 14, 2011
Over the next few years, astronomers will be able to observe first-hand how the super massive black hole at the centre of our Milky Way is being fed: an international team of astronomers led by the Max Planck Institute for Extraterrestrial Physics has found a gas cloud that is falling towards the black hole in the galactic centre. While some distortion due to the huge gravitational pull of the black hole can already be seen, the gas cloud will be completely disrupted and ultimately swallowed by the black hole, resulting in largely increased X-ray emission. The observations and analysis are described in a Nature paper, published online on 14 December 2011.
For more information see
MPE Press Release.
Caught in the act: Herschel detects gigantic storms sweeping entire galaxies clean
May 09, 2011
With observations from the PACS instrument on board the ESA Herschel space observatory, an international team of scientists led by the Max Planck Institute for Extraterrestrial Physics have found gigantic storms of molecular gas gusting in the centres of many galaxies. Some of these massive outflows reach velocities of more than 1000 kilometres per second, i.e. thousands of times faster than in terrestrial hurricanes. The observations show that the more active galaxies contain stronger winds, which can blow away the entire gas reservoir in a galaxy, thereby inhibiting both further star formation and the growth of the central black hole. This finding is the first conclusive evidence for the importance of galactic winds in the evolution of galaxies.
For more information see
MPE Press Release.