Wine and Cheese Fall 2021 - Revision history

Kdkuntz at 13:44, 10 December 2021

2021-12-10T13:44:23Z

← Older revision		Revision as of 13:44, 10 December 2021
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	'''Glimpsing the Compositions of Sub-Neptune-Size Worlds'''<br>		'''Glimpsing the Compositions of Sub-Neptune-Size Worlds'''<br>
	Sub-Neptune and super-Earth-size planets are a new category of astrophysical objects. Though absent from the Solar System, exoplanet surveys have revealed that they are a dominant outcome of planet formation found in abundance around other stars. The nature of these planets is not well understood. In the sub-Neptune size range a large variety of planet bulk compositions are a priori possible, including terrestrial super-Earths, mini-Neptunes with hydrogen-helium envelopes, and water-worlds with several tens of percent water by mass. In this talk, I will present recent results from my group aimed at understanding the nature and origin of these enigmatic sub-Neptune-size worlds and disentangling the relative contributions from various compositional scenarios to the observed population of planets.		Sub-Neptune and super-Earth-size planets are a new category of astrophysical objects. Though absent from the Solar System, exoplanet surveys have revealed that they are a dominant outcome of planet formation found in abundance around other stars. The nature of these planets is not well understood. In the sub-Neptune size range a large variety of planet bulk compositions are a priori possible, including terrestrial super-Earths, mini-Neptunes with hydrogen-helium envelopes, and water-worlds with several tens of percent water by mass. In this talk, I will present recent results from my group aimed at understanding the nature and origin of these enigmatic sub-Neptune-size worlds and disentangling the relative contributions from various compositional scenarios to the observed population of planets.

			=13 December=
			==Duncan Watts (UiO)==
			'''BeyondPlanck and Cosmoglobe: An End-to-End Bayesian Analysis of CMB Data'''<br>
			BeyondPlanck is a Bayesian reanalysis of the Planck Low Frequency Instrument (LFI) data. The framework performs Gibbs sampling for each stage of the data analysis pipeline, from raw diode data to maps of the galaxy and the Cosmic Microwave Background (CMB). BeyondPlanck is the first CMB analysis pipeline that explores the full posterior distribution of all parameters, including the properties of the instrument including gain, correlated noise, and bandpasses, to the astrophysical components and cosmological parameters. This allows for a proper error propagation and handling of correlations between various parameters along the analysis pipeline. I will present the results of the BeyondPlanck analysis, highlighting the improvements over the official Planck analysis pipeline, and pay special attention to the novel goodness-of-fit tests that we are able to perform in this framework.

			After summarizing the BeyondPlanck results, I will discuss the application of this framework to the WMAP data set, with particular emphasis on the Q-band data. I will show this as an example of the extendability of the Bayesian end-to-end formalism to external datasets beyond just the Planck LFI. This is the first step in the Cosmoglobe project, which will perform joint analysis of multiple datasets at once at the rawest level possible. I will close by describing the benefits of joint multi-experiment analyses in this form, and present the path of the Cosmoglobe project going forward.

Kdkuntz at 12:58, 2 December 2021

2021-12-02T12:58:28Z

← Older revision		Revision as of 12:58, 2 December 2021
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	=29 November=		=29 November=
	==Nicholas Kern==		==Nicholas Kern (MIT)==
	'''First Results from HERA Phase I: New Limits on the EoR 21 cm Power Spectrum'''<br>		'''First Results from HERA Phase I: New Limits on the EoR 21 cm Power Spectrum'''<br>
	Cosmic Dawn and the Epoch of Reionization (EoR) are crucial milestones in the growth of luminous structure and in the global picture of star and galaxy formation. Yet, to-date we currently have few direct constraints on exactly when and how these events took place. Hydrogen intensity mapping experiments hope to present a new picture of these processes by directly mapping the density, temperature, and ionization state of the intergalactic medium (IGM) from redshifts 6 < z < 30. However, significant technical challenges stand in the way of these measurements. Current experiments are addressing this with novel techniques for calibration, interference identification, and foreground and systematic modeling, leading to improved power spectrum upper limits. In this talk, I will discuss new limits set by the HERA experiment that improve upon existing limits at z=8 by over an order of magnitude in sensitivity. I will discuss key steps in the analysis that made this possible, the scientific impact of the limits, and future directions as HERA construction is completed and full-science observations commence.		Cosmic Dawn and the Epoch of Reionization (EoR) are crucial milestones in the growth of luminous structure and in the global picture of star and galaxy formation. Yet, to-date we currently have few direct constraints on exactly when and how these events took place. Hydrogen intensity mapping experiments hope to present a new picture of these processes by directly mapping the density, temperature, and ionization state of the intergalactic medium (IGM) from redshifts 6 < z < 30. However, significant technical challenges stand in the way of these measurements. Current experiments are addressing this with novel techniques for calibration, interference identification, and foreground and systematic modeling, leading to improved power spectrum upper limits. In this talk, I will discuss new limits set by the HERA experiment that improve upon existing limits at z=8 by over an order of magnitude in sensitivity. I will discuss key steps in the analysis that made this possible, the scientific impact of the limits, and future directions as HERA construction is completed and full-science observations commence.

			=6 December=
			==Leslie Rogers (Chicago)==
			'''Glimpsing the Compositions of Sub-Neptune-Size Worlds'''<br>
			Sub-Neptune and super-Earth-size planets are a new category of astrophysical objects. Though absent from the Solar System, exoplanet surveys have revealed that they are a dominant outcome of planet formation found in abundance around other stars. The nature of these planets is not well understood. In the sub-Neptune size range a large variety of planet bulk compositions are a priori possible, including terrestrial super-Earths, mini-Neptunes with hydrogen-helium envelopes, and water-worlds with several tens of percent water by mass. In this talk, I will present recent results from my group aimed at understanding the nature and origin of these enigmatic sub-Neptune-size worlds and disentangling the relative contributions from various compositional scenarios to the observed population of planets.

Kdkuntz at 19:03, 18 November 2021

2021-11-18T19:03:11Z

← Older revision		Revision as of 19:03, 18 November 2021
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	==John Soltis (JHU)==		==John Soltis (JHU)==
	'''Predicting Follow-Up Observations of Galaxy Clusters Using Machine Learning'''<be>		'''Predicting Follow-Up Observations of Galaxy Clusters Using Machine Learning'''<br>
	The eROSITA X-ray telescope, launched in 2019, is predicted to observe roughly 100,000 galaxy clusters. Our ability to follow up these observations with longer, higher resolution observations is expensive and limited, and objects for follow-up must be chosen with care. To aid in the evaluation of potential follow ups, we have developed a proof-of-concept algorithm for predicting longer, higher quality, observations based on mock eROSITA observations. We do so making use of the hydrodynamic cosmological simulation Magneticum, simulated eROSITA instrument conditions using SIXTE, and a novel convolutional neural network. We are able to closely predict radial luminosity profiles, remove noise, and capture substructure.		The eROSITA X-ray telescope, launched in 2019, is predicted to observe roughly 100,000 galaxy clusters. Our ability to follow up these observations with longer, higher resolution observations is expensive and limited, and objects for follow-up must be chosen with care. To aid in the evaluation of potential follow ups, we have developed a proof-of-concept algorithm for predicting longer, higher quality, observations based on mock eROSITA observations. We do so making use of the hydrodynamic cosmological simulation Magneticum, simulated eROSITA instrument conditions using SIXTE, and a novel convolutional neural network. We are able to closely predict radial luminosity profiles, remove noise, and capture substructure.

			=29 November=
			==Nicholas Kern==
			'''First Results from HERA Phase I: New Limits on the EoR 21 cm Power Spectrum'''<br>
			Cosmic Dawn and the Epoch of Reionization (EoR) are crucial milestones in the growth of luminous structure and in the global picture of star and galaxy formation. Yet, to-date we currently have few direct constraints on exactly when and how these events took place. Hydrogen intensity mapping experiments hope to present a new picture of these processes by directly mapping the density, temperature, and ionization state of the intergalactic medium (IGM) from redshifts 6 < z < 30. However, significant technical challenges stand in the way of these measurements. Current experiments are addressing this with novel techniques for calibration, interference identification, and foreground and systematic modeling, leading to improved power spectrum upper limits. In this talk, I will discuss new limits set by the HERA experiment that improve upon existing limits at z=8 by over an order of magnitude in sensitivity. I will discuss key steps in the analysis that made this possible, the scientific impact of the limits, and future directions as HERA construction is completed and full-science observations commence.

Kdkuntz at 19:56, 10 November 2021

2021-11-10T19:56:06Z

← Older revision		Revision as of 19:56, 10 November 2021
Line 65:		Line 65:
	The rapidly expanding field of the line intensity mapping (LIM) promises to revolutionise our understanding of the galaxy formation and evolution. Although primarily a tool for galaxy astrophysics, LIM technique can be used as a cosmological probe and I will point out one such application in rest of the talk. I will show that a linear combination of lensing maps from the cosmic microwave background (CMB) and from line intensity maps (LIMs) allows to exactly null the low-redshift contribution to CMB lensing, and extract only the contribution from the Universe from/beyond reionization. This would provide a unique probe of the Dark Ages, complementary with 21 cm. I will quantify the interloper bias (which is a key hurdle to LIM techniques) to LIM lensing for the first time, and derive a "LIM-pair" estimator which nulls it exactly.		The rapidly expanding field of the line intensity mapping (LIM) promises to revolutionise our understanding of the galaxy formation and evolution. Although primarily a tool for galaxy astrophysics, LIM technique can be used as a cosmological probe and I will point out one such application in rest of the talk. I will show that a linear combination of lensing maps from the cosmic microwave background (CMB) and from line intensity maps (LIMs) allows to exactly null the low-redshift contribution to CMB lensing, and extract only the contribution from the Universe from/beyond reionization. This would provide a unique probe of the Dark Ages, complementary with 21 cm. I will quantify the interloper bias (which is a key hurdle to LIM techniques) to LIM lensing for the first time, and derive a "LIM-pair" estimator which nulls it exactly.
	In the end, I will show some results for prospects of observing the Doppler boosted CIB emission and its applications.		In the end, I will show some results for prospects of observing the Doppler boosted CIB emission and its applications.

			=15 November=
			==Yuanze Luo (JHU)==
			'''A Multiwavelength view of IC 860: What Is in Action inside Quenching Galaxies'''<br>
			Observations of the galaxy population throughout the cosmic time have suggested an evolution scenario where galaxies evolve from blue and star-forming, to red and quiescent as star formation is quenched and gas is consumed in stars or becomes unavailable for stellar synthesis. The absence of a significant population falling in the intermediate region implies that these transitions must occur quite rapidly. Though multiple mechanisms have been shown to be able to quench galaxies in different ways, the interplay and relative importance of these mechanisms are still not fully understood. In this work, we study a particular quenching galaxy: IC 860, for which we have exquisite multiwavelength data to probe different activities such as outflows and AGN in the galaxy. IC 860 is a quenching galaxy at a very early stage and is therefore an ideal case study for understanding the triggers of quenching. Our analysis has confirmed the existence of multiphase outflows (in neutral and molecular gas), revealed evidence for a recent merger and the presence of a buried AGN, and supports the quenching picture where outflows help suppress star formation by disturbing rather than expelling all of the gas.

			==Rui Shi (JHU)==
			'''SMICA and its Application on CLASS-like Data'''<br>
			The Cosmology Large Angular Scale Surveyor (CLASS) is a ground-based telescope array in the Atacama Desert, aiming at measuring the largest scales of the cosmic microwave background (CMB) polarization to study early universe physics. CLASS has been observing the 75% of the sky since 2016, and now data from all of the four bands (40, 90, 150, 220 GHz) are being processed. One of the final steps in the analysis is component separation, by which the microwave frequency maps, contaminated by Galactic emission, are filtered and combined to separate out the pure CMB information. I will talk about my ongoing project to apply the Spectral Matching Independent Component Analysis (SMICA, a specific type of component separation method) to CLASS-like data.

			==John Soltis (JHU)==
			'''Predicting Follow-Up Observations of Galaxy Clusters Using Machine Learning'''<be>
			The eROSITA X-ray telescope, launched in 2019, is predicted to observe roughly 100,000 galaxy clusters. Our ability to follow up these observations with longer, higher resolution observations is expensive and limited, and objects for follow-up must be chosen with care. To aid in the evaluation of potential follow ups, we have developed a proof-of-concept algorithm for predicting longer, higher quality, observations based on mock eROSITA observations. We do so making use of the hydrodynamic cosmological simulation Magneticum, simulated eROSITA instrument conditions using SIXTE, and a novel convolutional neural network. We are able to closely predict radial luminosity profiles, remove noise, and capture substructure.

Kdkuntz at 15:27, 29 October 2021

2021-10-29T15:27:42Z

@@ Line 51: / Line 51: @@
 =25 October=
 ==Elena Murchikova (IAS)==
-'''Sagittarius A* in its Natural Habitat'''
+'''Sagittarius A* in its Natural Habitat'''<br>
 The Milky Way’s Galactic Center black hole Sagittarius A* is the supermassive black hole closest to us and has the largest angular size on the sky. Despite its proximity, the accretion flow onto it is not well understood. At large scales (0.05 pc and beyond), the primary source of information about accretion flow comes from observations of hot X-ray emitting gas. At near horizon scales, the density of the flow is constrained by submm polarization measurements. At intermediate scales, there are too few model-independent probes to reliably determine physical properties of the gas. In 2019, using ALMA observations I discovered a disk of relatively cool (T=10^4K) gas at intermediate distances (0.01 pc) from the black hole. The cool gas can be observed with much higher spatial resolution than the hot X-ray emitting gas, providing new probes of the inner accretion flow of the Sagittarius A*. In this talk I will review what is known about the structure of the accretion flow around Sgr A*, and I will summarize my ongoing research program to determine the origin and the physical conditions of the cool gas and its contribution the accretion onto our local supermassive black hole.

Kdkuntz at 20:29, 21 October 2021

2021-10-21T20:29:18Z

← Older revision		Revision as of 20:29, 21 October 2021
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	'''Measuring Massive Star Embeddedness in the Andromeda Galaxy'''<br>		'''Measuring Massive Star Embeddedness in the Andromeda Galaxy'''<br>
	Massive stars interact with their surrounding interstellar medium (ISM) via dynamically disruptive feedback mechanisms. By studying their relative embeddedness, we can start to constrain the 3D distribution of the ISM, bridging the gap between observation and massive star feedback simulations.		Massive stars interact with their surrounding interstellar medium (ISM) via dynamically disruptive feedback mechanisms. By studying their relative embeddedness, we can start to constrain the 3D distribution of the ISM, bridging the gap between observation and massive star feedback simulations.

			=25 October=
			==Elena Murchikova (IAS)==
			'''Sagittarius A* in its Natural Habitat'''
			The Milky Way’s Galactic Center black hole Sagittarius A* is the supermassive black hole closest to us and has the largest angular size on the sky. Despite its proximity, the accretion flow onto it is not well understood. At large scales (0.05 pc and beyond), the primary source of information about accretion flow comes from observations of hot X-ray emitting gas. At near horizon scales, the density of the flow is constrained by submm polarization measurements. At intermediate scales, there are too few model-independent probes to reliably determine physical properties of the gas. In 2019, using ALMA observations I discovered a disk of relatively cool (T=10^4K) gas at intermediate distances (0.01 pc) from the black hole. The cool gas can be observed with much higher spatial resolution than the hot X-ray emitting gas, providing new probes of the inner accretion flow of the Sagittarius A. In this talk I will review what is known about the structure of the accretion flow around Sgr A, and I will summarize my ongoing research program to determine the origin and the physical conditions of the cool gas and its contribution the accretion onto our local supermassive black hole.

Kdkuntz: /* 18 October= */

2021-10-15T03:50:15Z

18 October=

← Older revision		Revision as of 03:50, 15 October 2021
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	Next generation cosmic microwave background (CMB) experiments and galaxy surveys will generate a wealth of new data with unprecedented precision on small scales. Correlations between CMB anisotropies and the galaxy density carry valuable cosmological information about the largest scales, creating novel opportunities for inference. In this talk I will discuss the science goals for the kinetic Sunyaev Zel’dovich (kSZ) and the moving-lens effects and describe the method of velocity tomography which allows recovering large-scale cosmological information from the measurements of small scales.		Next generation cosmic microwave background (CMB) experiments and galaxy surveys will generate a wealth of new data with unprecedented precision on small scales. Correlations between CMB anisotropies and the galaxy density carry valuable cosmological information about the largest scales, creating novel opportunities for inference. In this talk I will discuss the science goals for the kinetic Sunyaev Zel’dovich (kSZ) and the moving-lens effects and describe the method of velocity tomography which allows recovering large-scale cosmological information from the measurements of small scales.

	=18 October==		=18 October=
	==Yuzo Ishikawa (JHU)==		==Yuzo Ishikawa (JHU)==
	'''Exploring the Impact of Quasars on Galaxy Evolution and its Environments'''<br>		'''Exploring the Impact of Quasars on Galaxy Evolution and its Environments'''<br>

Kdkuntz at 03:50, 15 October 2021

2021-10-15T03:50:02Z

← Older revision		Revision as of 03:50, 15 October 2021
Line 39:		Line 39:
	'''Fundamental Physics from Velocity Tomography'''<br>		'''Fundamental Physics from Velocity Tomography'''<br>
	Next generation cosmic microwave background (CMB) experiments and galaxy surveys will generate a wealth of new data with unprecedented precision on small scales. Correlations between CMB anisotropies and the galaxy density carry valuable cosmological information about the largest scales, creating novel opportunities for inference. In this talk I will discuss the science goals for the kinetic Sunyaev Zel’dovich (kSZ) and the moving-lens effects and describe the method of velocity tomography which allows recovering large-scale cosmological information from the measurements of small scales.		Next generation cosmic microwave background (CMB) experiments and galaxy surveys will generate a wealth of new data with unprecedented precision on small scales. Correlations between CMB anisotropies and the galaxy density carry valuable cosmological information about the largest scales, creating novel opportunities for inference. In this talk I will discuss the science goals for the kinetic Sunyaev Zel’dovich (kSZ) and the moving-lens effects and describe the method of velocity tomography which allows recovering large-scale cosmological information from the measurements of small scales.

			=18 October==
			==Yuzo Ishikawa (JHU)==
			'''Exploring the Impact of Quasars on Galaxy Evolution and its Environments'''<br>
			Quasars are believed to play an important role in the formation and evolution of galaxies. Their powerful radiation is often invoked to drive quasar feedback, impacting evolution in the galactic to intergalactic scales across cosmic history. I will give an overview of my recent projects exploring the various ways quasars affect these regimes. X-rays probes the radiation from the accretion disk of the central black hole, and deep near-IR imaging probes the earliest quasars at the End of Reionization. Current and future advances in spatially resolved spectroscopy will allow detailed characterization of the quasars' impact.

			==Christina Lindberg (JHU)==
			'''Measuring Massive Star Embeddedness in the Andromeda Galaxy'''<br>
			Massive stars interact with their surrounding interstellar medium (ISM) via dynamically disruptive feedback mechanisms. By studying their relative embeddedness, we can start to constrain the 3D distribution of the ISM, bridging the gap between observation and massive star feedback simulations.

Kdkuntz: /* Selim Hotinli(JHU) */

2021-10-08T15:18:19Z

Selim Hotinli(JHU)

← Older revision		Revision as of 15:18, 8 October 2021
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	Type Ia supernovae (SNe Ia) are important cosmological probes due to their standardizable nature. In order to obtain distance measurements of SNe Ia, the SN Ia light curves are traditionally fitted to an empirical light curve model. As we gain better knowledge on the various systematics in SN Ia cosmology analysis, the modeling uncertainty will likely become the largest in the near future. I will describe various ways the model training procedure can potentially bias the final cosmological constraints, and discuss improvements we can make to reduce these biases.		Type Ia supernovae (SNe Ia) are important cosmological probes due to their standardizable nature. In order to obtain distance measurements of SNe Ia, the SN Ia light curves are traditionally fitted to an empirical light curve model. As we gain better knowledge on the various systematics in SN Ia cosmology analysis, the modeling uncertainty will likely become the largest in the near future. I will describe various ways the model training procedure can potentially bias the final cosmological constraints, and discuss improvements we can make to reduce these biases.

	==Selim Hotinli(JHU)==		==Selim Hotinli (JHU)==
	'''Fundamental Physics from Velocity Tomography'''<br>		'''Fundamental Physics from Velocity Tomography'''<br>
	Next generation cosmic microwave background (CMB) experiments and galaxy surveys will generate a wealth of new data with unprecedented precision on small scales. Correlations between CMB anisotropies and the galaxy density carry valuable cosmological information about the largest scales, creating novel opportunities for inference. In this talk I will discuss the science goals for the kinetic Sunyaev Zel’dovich (kSZ) and the moving-lens effects and describe the method of velocity tomography which allows recovering large-scale cosmological information from the measurements of small scales.		Next generation cosmic microwave background (CMB) experiments and galaxy surveys will generate a wealth of new data with unprecedented precision on small scales. Correlations between CMB anisotropies and the galaxy density carry valuable cosmological information about the largest scales, creating novel opportunities for inference. In this talk I will discuss the science goals for the kinetic Sunyaev Zel’dovich (kSZ) and the moving-lens effects and describe the method of velocity tomography which allows recovering large-scale cosmological information from the measurements of small scales.

Kdkuntz at 15:17, 8 October 2021

2021-10-08T15:17:59Z

← Older revision		Revision as of 15:17, 8 October 2021
Line 30:		Line 30:
	'''“Mockulus reparo” – to Fix the Effects on Metallicity Gradient Measurements Due to Our Insufficient “Seeing”'''<br>		'''“Mockulus reparo” – to Fix the Effects on Metallicity Gradient Measurements Due to Our Insufficient “Seeing”'''<br>
	Gas-phase metallicity gradients of galaxies are a crucial ingredient for understanding the chemical evolution of galaxies. However, measurements of gradients are often affected by limited spatial resolution. The extent of this effect may be different across observations, making cross-observation comparisons unreliable. We produce mock IFU datacubes from hydrodynamic simulations of an isolated galaxy and use those to quantify the said effect. I will present the application of our models on current IFU surveys — MaNGA, SAMI and CALIFA — by correcting the observed metallicity gradients for the effects of spatial resolution. I will demonstrate that while the mean trend of metallicity gradient versus stellar mass is largely unaffected, individual galaxies can undergo significant corrections. Our proposed method of correcting metallicity gradients by using isolated galaxy simulations already enables meaningful cross-survey comparisons. However, the next goal is to produce mock datacubes of cosmological simulations, in order to sample a broad range of galaxy properties. In this regard, I will briefly highlight some of my current efforts to study the metallicity distributions in the FOGGIE simulations.		Gas-phase metallicity gradients of galaxies are a crucial ingredient for understanding the chemical evolution of galaxies. However, measurements of gradients are often affected by limited spatial resolution. The extent of this effect may be different across observations, making cross-observation comparisons unreliable. We produce mock IFU datacubes from hydrodynamic simulations of an isolated galaxy and use those to quantify the said effect. I will present the application of our models on current IFU surveys — MaNGA, SAMI and CALIFA — by correcting the observed metallicity gradients for the effects of spatial resolution. I will demonstrate that while the mean trend of metallicity gradient versus stellar mass is largely unaffected, individual galaxies can undergo significant corrections. Our proposed method of correcting metallicity gradients by using isolated galaxy simulations already enables meaningful cross-survey comparisons. However, the next goal is to produce mock datacubes of cosmological simulations, in order to sample a broad range of galaxy properties. In this regard, I will briefly highlight some of my current efforts to study the metallicity distributions in the FOGGIE simulations.

			=11 October=
			==Mi Dai (JHU)==
			'''Understanding the Systematics in Type Ia Supernova Modeling for Cosmology'''<br>
			Type Ia supernovae (SNe Ia) are important cosmological probes due to their standardizable nature. In order to obtain distance measurements of SNe Ia, the SN Ia light curves are traditionally fitted to an empirical light curve model. As we gain better knowledge on the various systematics in SN Ia cosmology analysis, the modeling uncertainty will likely become the largest in the near future. I will describe various ways the model training procedure can potentially bias the final cosmological constraints, and discuss improvements we can make to reduce these biases.

			==Selim Hotinli(JHU)==
			'''Fundamental Physics from Velocity Tomography'''<br>
			Next generation cosmic microwave background (CMB) experiments and galaxy surveys will generate a wealth of new data with unprecedented precision on small scales. Correlations between CMB anisotropies and the galaxy density carry valuable cosmological information about the largest scales, creating novel opportunities for inference. In this talk I will discuss the science goals for the kinetic Sunyaev Zel’dovich (kSZ) and the moving-lens effects and describe the method of velocity tomography which allows recovering large-scale cosmological information from the measurements of small scales.