WELCOME TO MY TECHNICAL UNIVERSE

My research is focused on precision cosmology, e.g., combining theoretical work with new measurements to place sharp constraints on cosmological models and their free parameters. (Skip to here if you already know all this.) Spectacular new measurements are providing powerful tools for this:

So far, I've worked mainly on CMB, LSS and 21 cm tomography, with some papers involving lensing, SN Ia and LyAF as well.

Why do I find cosmology exciting?
(Even if you don't find cosmology exciting, there are good reasons why you should support physics research.)

1. There are some very basic questions that still haven't been answered. For instance,
• Is really only 4% of our universe made of atoms? So it seems, but what precisely is the weird "dark matter" and "dark energy" that make up the rest?
• Will the Universe expand forever or end in a cataclysmic crunch or big rip? The smart money is now on the first option, but the jury is still out.
• How did it all begin, or did it? This is linked to particle phyiscs and unifying gravity with quantum theory.
• Are there infinitely many other stars, or does space connect back on itself? Most of my colleagues assume it is infinite and the data supports this, but we don't know yet.
2. Thanks to an avalanche of great new data, driven by advances in satellite, detector and computer technology, we may be only years away from answering some of these questions.

Since our atmosphere messes up most electromagnetic waves coming from space (the main exceptions being radio waves and visible light), the advent of satellites has revolutionized our ability to photograph the Universe in microwaves, infrared light, ultraviolet light, X-rays and gamma rays. New low-temperature detectors have greatly improved what can be done from the ground as well, and the the computer revolution has enabled us to gather and process huge data quantities, doing research that would have been unthinkable twenty years ago. This data avalanche has transformed cosmology from being a mainly theoretical field, occasionally ridiculed as speculative and flaky, into a data-driven quantitative field where competing theories can be tested with ever-increasing precision. I find CMB, LSS, lensing, SN Ia, LyAF, clusters and BBN to be very exciting areas, since they are all being transformed by new high-precision measurements as described below. Since each of them measures different but related aspects of the Universe, they both complement each other and allow lots of cross-checks.

What are these cosmological parameters?
In our standard cosmological model, the Universe was once in an extremely dense and hot state, where things were essentially the same everywhere in space, with only tiny fluctuations (at the level of 0.00001) in the density. As the Universe expanded and cooled, gravitational instability caused these these fluctuations to grow into the galaxies and the large-scale structure that we observe in the Universe today. To calculate the details of this, we need to know about a dozen numbers, so-called cosmological parameters. Most of these parameters specify the cosmic matter budget, i.e., what the density of the Universe is made up of - the amounts of the following ingredients:

• Baryons - the kind of particles that you and I and all the chemical elements we learned about in school are made of: protons & neutrons. Baryons appear to make up only about 5% of all stuff in the Universe.
• Photons - the particles that make up light. Their density is the best measured one on this list.
• Massive neutrinos - neutrinos are very shy particles. They are known to exist, and now at least two of the three or more kinds are known to have mass.
• Cold dark matter - unseen mystery particles widely believed to exist. There seems to be about five times more of this strange stuff than baryons, making us a minority in the Universe.
• Curvature - if the total density differs from a certain critical value, space will be curved. Sufficiently high density would make space be finite, curving back on itself like the 3D surface of a 4D hypersphere.
• Dark energy - little more than a fancy name our ignorance of what seems to make up about two thirds of the matter budget. One popular candidates is a "Cosmological constant", a.k.a. Lambda, which Einstein invented and then later called his greatest blunder. Other candidates are more complicated modifications to Einsteins theory of Gravity as well as energy fields known as "quintessence". Dark energy causes gravitational repulsion in place of attraction. Einstein invented it and called it his greatest mistake, but combining new SN Ia and CMB data indicates that we might be living with Lambda after all.

Then there are a few parameters describing those tiny fluctuations in the early Universe; exactly how tiny they were, the ratio of fluctuations on small and large scales, the relative phase of fluctuations in the different types of matter, etc. Accurately measuring these parameters would test the most popular theory for the origin of these wiggles, known as inflation, and teach us about physics at much higher energies than are accessible with particle accelerator experiments. Finally, there are a some parameters that Dick Bond, would refer to as "gastrophysics", since they involve gas and other ghastly stuff. One example is the extent to which feedback from the first galaxies have affected the CMB fluctuations via reionization. Another example is bias, the relation between fluctuations in the matter density and the number of galaxies.

One of my main current interests is using the avalanche of new data to raise the ambition level beyond cosmological parameters, testing rather than assuming the underlying physics. My battle cry is published here with nuts and bolts details here and here.

The cosmic toolbox
Here is a brief summary of some key cosmological observables and what they can teach us about cosmological parameters.

Photos of the cosmic microwave background (CMB) radiation like the one to the left show us the most distant object we can see: a hot, opaque wall of glowing hydrogen plasma about 14 billion light years away. Why is it there? Well, as we look further away, we're seeing things that happened longer ago, since it's taken the light a long time to get here. We see the Sun as it was eight minutes ago, the Andromeda galaxy the way it was a few million years ago and this glowing surface as it was just 400,000 years after the Big Bang. We can see that far back since the hydrogen gas that fills intergalactic space is transparent, but we can't see further, since earlier the hydrogen was so hot that it was an ionized plasma, opaque to light, looking like a hot glowing wall just like the surface of the Sun. The detailed patterns of hotter and colder spots on this wall constitute a goldmine of information about the cosmological parameters mentioned above. If you are a newcomer and want an introduction to CMB fluctuations and what we can learn from them, I've written a review here. If you don't have a physics background, I recommend the on-line tutorials by Wayne Hu and Ned Wright. Two new promising CMB fronts are opening up --- CMB polarization and arcminute scale CMB, and are likely to keep the CMB field lively for at leastr another decade.

Large-scale structure: 3D mapping of the Universe with galaxy redshift surveys offers another window on dark matter properties, through its gravitational effects on galaxy clustering. This field is currently being transformed by everr larger Galaxy Redshift Survey. I've had lots of fun working with my colleagues on the Sloan Digital Sky Survey (SDSS) to carefully analyze the gargantuan galaxy maps and work out what they tell us about our cosmic composition, origins and ultimate fate. The abundance of galaxy clusters, the largest gravitationally bound and equilibrated blobs of stuff in the Universe, is a very sensitive probe of both the cosmic expansion history and the growth of matter clustering. Many powerful cluster finding techniques are contributing to rapid growth in the number of known clusters and our knowledge of their properties: identifying them in 3D galaxy surveys, seeing their hot gas as hot spots in X-ray maps or cold spots in microwave maps (the so-called SZ-effect) or spotting their gravitational effects with gravitational lensing.

Yet another probe of dark matter is offered by gravitational lensing, whereby its gravitational pull bends light rays and distorts images of distant objects. The first large-scale detections of this effect were reported by four groups (astro-ph/0002500, 0003008, 0003014, 0003338) in the year 2000, and I anticipate making heavy use of such measurements as they continue to improve, partly in collaboration with Bhuvnesh Jain at Penn. Lensing is ultimately as promising as CMB and is free from the murky bias issues plaguing LSS and LyAF measurements, since it probes the matter density directly via its gravitational pull. I've also dabbled some in the stronger lensing effects caused by galaxy cores, which offer additional insights into the detailed nature of the dark matter.

Supernovae Ia: If a white dwarf (the corpse of a burned-out low-mass star like our Sun) orbits another dying star, it may gradually steal its gas and exceed the maximum mass with which it can be stable. This makes it collapse under its own weight and blow up in a cataclysmic explosion called a supernova of type Ia. Since all of these cosmic bombs weigh the same when they go off (about 1.4 solar masses, the so-called Chandrasekhar mass), they all release roughly the same amount of energy - and a more detailed calibration of this energy is possible by measuring how fast it dims, making it the best "standard candle" visible at cosmological distances. The supernova cosmology project and the high z SN search team mapped out how bright SN Ia looked at different redshifts found the first evidence in 1998 that the expansion of the Universe was accelerating. This approach can ultimately provide a direct measurement of the density of the Universe as a function of time, helping unravel the nature of dark energy - I hope the SNAP project or one of its competitores gets funded. The image to the left resulted from a different type of supernova, but I couldn't resist showing it anyway...

The so-called Lyman Alpha Forest, cosmic gas clouds backlit by quasars, offers yet another new and exciting probe of how dark has clumped ordinary matter together, and is sensitive to an epoch when the Universe was merely 10-20% of its present age. Although relating the measured absorption to the densities of gas and dark matter involves some complications, it completely circumvents the Pandora's of galaxy biasing. Cosmic observations are rapidly advancing on many other fronts as well, e.g., with direct measurements of the cosmic expansion rate and the cosmic baryon fraction.

Summary of my past and current cosmology research
I used to have a description of each of my papers on this page, but it got very boring to read as the numbers grew, so I moved most of it to here. After graduate work on the role of atomic and molecular chemistry in cosmic reionization, I have mainly focused my research on issues related to constraining cosmological models. A suite of papers developed methods for analyzing cosmological data sets and applied them to various CMB experiments and galaxy redshift surveys, often in collaboration with the experimentalists who had taken the data. Another series of papers tackled various "dirty laundry" issues such as microwave foregrounds and mass-to-light bias. Other papers like this one develop and apply techniques for clarifying the big picture in cosmology: comparing and combining diverse cosmological probes, cross-checking for consistency and constraining cosmological models and their free parameters. (The difference between cosmology and ice hockey is that I don't get penalized for cross-checking...) My main current research interest is cosmology theory and phenomenology. I'm particularly enthusiastic about the prospects of comparing and combining current and upcoming data on CMB, LSS, galaxy clusters, lensing, LyA forest clustering, SN 1, 21 cm tomography, etc. to raise the ambition level beyond the current cosmological parameter game, testing rather than assuming the underlying physics. This paper contains my battle cry. I also retain a strong interest in low-level nuts-and-bolts analysis and interpretation of data, firmly believing that the devil is in the details, and am actively working on neutral hydrogen tomography theory, experiment and data analysis for our Omniscope project - I hope to find time to write more about that here soon.

OTHER RESEARCH: SIDE INTERESTS
Early galaxy formation and the end of the cosmic dark ages
One of the main challenges in modern cosmology is to quantify how small density fluctuations at the recombination epoch at redshift around z=1000 evolved into the galaxies and the large-scale structure we observe in the universe today. My Ph.D. thesis with Joe Silk focused on ways of probing the interesting intermediate epoch. The emphasis was on the role played by non-linear feedback, where a small fraction of matter forming luminous objects such as stars or QSO's can inject enough energy into their surrounding to radically alter subsequent events. We know that the intergalactic medium (IGM) was reionized at some point, but the details of when and how this occurred remain open. The absence of a Gunn-Peterson trough in the spectra of high-redshift quasars suggests that it happened before z=5, which could be achieved through supernova driven winds from early galaxies. Photoionization was thought to be able to partially reionize the IGM much earlier, perhaps early enough to affect the cosmic microwave background (CMB) fluctuations, especially in an open universe. However, extremely early reionization is ruled out by the COBE FIRAS constraints on the Compton y-distortion. To make predictions for when the first objects formed and how big they were, you need to worry about something I hate: molecules. Although I was so fed up with rate discrepancies in the molecule literature that I verged on making myself a Ghostbuster-style T-shirt reading "MOLECULES - JUST SAY NO", the irony is that my molecule paper that I hated so much ended up being one of my most cited ones. Whereas others that I had lots of fun with went largely unnoticed...

Gamma-ray bursts
Like most everybody else, I'm mystified and intrigued by the origin of gamma-ray bursts. Applying some of my power-spectrum related data analysis techniques to the new BATSE 3B data set, I have helped sharpen previous upper limits on anisotropy on all angular scales as well as tighten the previous best limits on burst repetition. Since these new limits were quite difficult to accommodate in models with a galactic halo origin, I firmly believed that gamma-ray bursts originated at cosmologically large distances from us - and I'm glad that I believed this before May 1997, when the halo camp finally conceded defeat! (Absorption lines with redshift 0.8 were detected in the afterglow of a gamma-ray burst.)

Quantum decoherence
I have a side interest in quantum decoherence - if you'd like to know more about what this is, check out my recent article in with John Archibald Wheeler in Scientific American here. I'm interested in decoherence both for its quantitative implications for quantum computing etc and for its philosophical implications for the interpretation of quantum mechanics. For much more on this wackier side of mine, click the banana icon above. Since macroscopic systems are virtually impossible to isolate from their surroundings, a number of quantitative predictions can be made for how their wavefunction will appear to collapse, in good agreement with what we in fact observe. Similar quantitative predictions can be made for models of heat baths, showing how the effects of the environment cause the familiar entropy increase and apparent directionality of time. Intriguingly, decoherence can also be shown to produce generalized coherent states, indicating that these are not merely a useful approximation, but indeed a type of quantum states that we should expect nature to be full of. All these changes in the quantum density matrix can in principle be measured experimentally, with phases and all.

Math problems
I'm also interested in physics-related mathematics problems in general. For instance, if you don't believe that part of a constrained elliptic metal sheet may bend towards you if you try to push it away, you are making the same mistake that the famous mathematician Hadamard once did.

Crazy stuff
I also have a wild side, which is why my friends call me Mad Max. Your can read about my more far-out research here. Ironically, the cosmology stuff described above also used to be considered flaky not to long ago, but times have changed!

MY RESEARCH GROUP

I've given birth to three Ph.D.'s at Penn: from left to right, they are David Rusin (left for postdoc at Harvard in 2001), Yongzhong Xu (left for postdoc at LANL in 2003) and Xiaomin Wang (left for postdoc at Chicago in 2004). I still haven't extorted photos from my two postdocs Havard Sandvik and Jose-Maria "Chema" Diego. Here's my research group at MIT in April 2008, in my office. In the order you'd read a book, you're looking at Yi Mao (left for postdoc in Austin), Courtney Peterson (still a grad student), Leslie Rogers (still a grad student), Robert Moffat (undergrad, left to do grad school in Stanford), Alexandra Rahlin (undergrad, left to do grad school in Princeton), Molly Swanson (left for postdoc at University College in London), Adrian Liu (still a grad student), Colin Hill (undergrad, left for grad school in Princeton), yours truly, and Mark Hertzberg (still a grad student). Here are my astro colleagues at MIT.

MY PUBLICATIONS
Please click on any paper that you want more information about. Most of these papers are rather technical, so if you're not too into equations and science jargon, you might find these popular articles more fun. There's a brief overview of all these articles and how they fit together at the bottom of this page. If you, in the Google spirit, care about what other people care about, here's my citation summary.

Cosmology publications

1. Late reionization by supernova-driven winds
   M Tegmark, J Silk & A Evrard 1993, ApJ, 417, 54-62
2. On the inevitability of reionization: implications for cosmic microwave background fluctuations
   M Tegmark, J Silk & A Blanchard 1994, ApJ, 420, 484-496
3. Did the universe recombine? New spectral constraints on reheating
   M Tegmark & J Silk 1994, ApJ, 423, 529-533
4. Power spectrum independent constraints on cosmological models
   M Tegmark, E Bunn & W Hu 1994, ApJ, 434, 1-11
5. New Constraints on Reionization from the Compton y-parameter
   M Tegmark & J Silk 1994, In Present and Future of the cosmic microwave background radiation, In Present and Future of the cosmic microwave background radiation, Eds. L. Cayon, E. Martinez-Gonzales & J. Sanz, Springer Verlag Gonzales & J. Sanz, Springer Verlag
6. Probes of the early universe
   M Tegmark, Ph.D. thesis, U. C. Berkeley, Dept. of Physics, May 1994
7. Reconstructing cosmic fields from redshift data - an explicit solution for the linear regime
   M Tegmark 1995, Nucl. Phys. B, S43, 295-298
8. Reionization in an open CDM universe: implications for cosmic microwave background fluctuations
   M Tegmark & J Silk 1995, ApJ, 441, 458-464
9. Estimating microwave power spectra
   M Tegmark 1995, Ann. N.Y. Acad. Sci., 759, 684-687
10. Real-space cosmic fields from redshift-space distributions: a Green function approach
    M Tegmark & B Bromley 1995, ApJ, 453, 533-540
11. A brute-force analysis of the COBE data
    M Tegmark & E Bunn 1995, ApJ, 455, 1-6
12. A method for extracting maximum resolution power spectra from microwave sky maps
    M Tegmark 1996, MNRAS, 280, 299-308
13. A method for extracting maximum resolution power spectra from galaxy surveys
    M Tegmark 1995, ApJ, 455, 429-438
14. Making the most of galaxy surveys: an optimal method for power spectrum estimation
    M Tegmark 1995, in proceedings of Max-Planck-Gesellschaft 1996 Ringberg Workshop
15. Estimating power spectra from 3D galaxy surveys
    M Tegmark 1995, in `Proceedings of the XXXth Rencontres de Moriond: Clustering in the universe, Eds. S Maurogordato et al, p49
16. Using the kinematic Sunyaev-Zeldovich effect to determine the peculiar velocities of clusters of galaxies
    M Haehnelt & M Tegmark 1996, MNRAS, 279, 545-556
17. A method for subtracting foregrounds from multi-frequency CMB sky maps
    M Tegmark & G P Efstathiou 1996, MNRAS, 281, 1297-1314
18. Spherical harmonic analysis of the angular distribution of GRBs
    M. Tegmark, D. H. Hartmann, M. S. Briggs & C. A. Meegan 1996, in Proc. 3rd Huntsville workshop on Gamma Ray Bursts.
19. The angular power spectrum of BATSE 3B gamma-ray bursts
    M Tegmark, D H Hartmann, M S Briggs & C A Meegan 1996, ApJ, 468, 214-224
20. Improved limits on gamma ray burst repetition
    M Tegmark, D H Hartmann, M S Briggs, Jon Hakkila & C A Meegan 1996, ApJ, 466, 757-763
21. Doppler peaks and all that: CMB anisotropies and what they can tell us
    M Tegmark 1996, lecture notes in Proc. Enrico Fermi, Course CXXXII, Varenna
22. The angular power spectrum of the 4 year COBE data
    M Tegmark 1996, ApJ Lett, 464, L35-L38
23. How small were the first cosmological objects?
    M Tegmark, J Silk, M J Rees, A Blanchard, T Abel & F Palla 1997, ApJ, 474, 1-12
24. Karhunen-Loeve eigenvalue problems in cosmology: how to tackle large data sets?
    M Tegmark, A N Taylor, & A F Heavens 1997, ApJ, 480, 22-35
25. An improved method for pixelizing CMB sky maps
    M Tegmark 1997, in Microwave Background Anisotropies, Eds. F Bouchet et al (Editions Frontieres), 475-480
26. An icosahedron-based method for pixelizing the celestial sphere
    M Tegmark 1996, ApJ Lett, 470, L81-L84
27. A high-resolution map of the cosmic microwave background around the north celestial pole
    M Tegmark, A de Oliveira-Costa, M J Devlin, C B Netterfield, L Page & E J Wollack 1997, ApJ Lett, 474, L77-L80
28. Is lensing of point sources a problem for future CMB experiments?
    M Tegmark & J V Villumsen 1997, MNRAS, 289, 169-174
29. Studies of CMB structure at Dec=+40. II: Analysis and cosmological interpretation
    S. Hancock, C. M. Gutierrez, R. D. Davies, A. N. Lasenby, G. Rocha, R. Rebolo, R. A. Watson & M. Tegmark 1997, MNRAS, 289, 505-514
30. How to make CMB maps without losing information
    M Tegmark 1997, ApJ Lett, 480, L87-L90
31. How to measure CMB power spectra without losing information
    M Tegmark 1997, Phys. Rev. D, 55, 5895-5907
32. Uncorrelated measurements of the CMB power spectrum
    M Tegmark & A J S Hamilton 1998, astro-ph/9702019, in proccedings of the 18th Texas Symposium on Relativistics Astrophysics & Cosmology, eds A V Olinto, J A Frieman & D N Schramm, p270-272 (World Scientific)
33. Forecasting cosmic parameter errors from microwave background anisotropy experiments
    J R Bond, G Efstathiou & M Tegmark 1997, MNRAS, 291, L33-L41
34. Analyzing redshift surveys to measure the power spectrum on large scales
    M Tegmark 1998, in Ringberg Workshop on Large-Scale Structure, ed. D. Hamilton (Kluwer, Amsterdam), preprint astro-ph/9708021
35. CMB mapping experiments: a designer's guide
    M Tegmark 1997, Phys. Rev. D, 56, 4514-4529
36. Cosmological parameter estimation from the CMB
    A Taylor, A Heavens, B Ballinger & M Tegmark 1997, in Proceedings of PPEUC97, Ed A Lasenby (Cambridge Univ. Press, Cambridge)
37. Measuring cosmological parameters with galaxy surveys
    M Tegmark 1997, Phys. Rev. Lett., 79, 3806-9
38. Measuring the galaxy power spectrum with future redshift surveys
    M Tegmark, A Hamilton, M Strauss, M Vogeley & A Szalay 1998, ApJ, 499, 555-576
39. Why is the CMB fluctuation level 10^-5?
    M Tegmark & M Rees 1998, ApJ, 499, 526-532
40. Cosmic microwave background maps from the HACME experiment
    M Tegmark, A de Oliveira-Costa, J Staren, P Meinhold, P Lubin, J Childers, N Figueiredo, T Gaier, M Lim, M Seiffert, T Villela & C A Wuensche 2000, ApJ, 541, 535-541
41. Removing real-world foregrounds from CMB maps
    M Tegmark 1998, ApJ, 502, 1-6
42. Weighing neutrinos with galaxy surveys
    W Hu, D J Eisenstein & M Tegmark 1998, Phys. Rev. Lett., 80, 5255-5258
43. Removing point sources from CMB maps
    M Tegmark & A de Oliveira-Costa 1998, ApJL, 500, 83-86
44. The time-evolution of bias
    M Tegmark & P J E Peebles 1998,  ApJL, 500, 79-82
45. Cosmic complementarity: combining CMB and supernova observations
    M Tegmark, D J Eisenstein & W Hu 1998, in "Fundamental parameters in Cosmology", Rencontres de Moriond
46. Cosmic complementarity: probing the acceleration of the Universe
    M Tegmark, D J Eisenstein,W Hu & R Kron 1998, astro-ph/9805117
47. Cosmic complementarity: H_0 and Omega_m from combining CMB experiments and redshift surveys
    D J Eisenstein,W Hu & M Tegmark 1998, astro-ph/9805239, ApJL, 504, L57-60
48. Observationally Determining the Properties of Dark Matter
    W Hu, D J Eisenstein, M Tegmark & M White 1999, astro-ph/9806362, Phys. Rev. D, 59, 023512
49. Cosmic Complementarity: Joint Parameter Estimation from CMB Experiments and Redshift Surveys
    D J Eisenstein,W Hu & M Tegmark 1999, astro-ph/9807130, ApJ, 518, 2-23
50. Galactic emission at 19 GHz
    A de Oliveira-Costa, M Tegmark, L Page & S Boughn 1998, astro-ph/9807329, ApJL, 509, L9-12
51. Mapping the CMB I: the first flight of the QMAP experiment
    M Devlin, A de Oliveira-Costa, T Herbig, A Miller, C  B Netterfield, L Page & M Tegmark 1998, astro-ph/9808043, ApJL, 509, L65-68
52.  Mapping the CMB II: the second flight of the QMAP experiment
    M Devlin, A de Oliveira-Costa, T Herbig, A Miller, L Page & M Tegmark 1998, astro-ph/9808044, ApJL, 509 L69-72
53.  Mapping the CMB III: combined analysis of QMAP flights
    A de Oliveira-Costa, M Devlin, T Herbig, A Miller, C  B Netterfield, L Page & M Tegmark 1998, astro-ph/9808045, ApJL, 509, L73-76
54. Cosmological constraints on neutrino masses
    M Tegmark, W Hu & D J Eisenstein 1998, in  proceedings of  1998 Ringberg Euroconference, Ed. Bernd Kniehl
55. Comparing and combining CMB datasets
    M Tegmark 1999, astro-ph/9809001, ApJL, 519, 513-517
56. Bias and beyond
    M Tegmark, astro-ph/9809185, in ``Wide Field Surveys in Cosmology'', S. Colombi and Y. Mellier (eds), Editions Frontieres (1998), p43-46
57. New techniques for making CMB maps
    A de Oliveira-Costa & M Tegmark, in ``Wide Field Surveys in Cosmology'', S. Colombi and Y. Mellier (eds), Editions Frontieres (1998), p311-314
58. Cosmological constraints from current CMB and SN Ia data: a brute force 8 parameter analysis
    M Tegmark 1999, astro-ph/9809201, ApJL, 514, L69-72
59. Observational evidence for stochastic biasing
    M Tegmark & B Bromley 1999, astro-ph/9809324,  ApJL, 518, L69-72
60. Weak lensing: prospects for measuring cosmological parameters
    W Hu & M Tegmark 1999, astro-ph/9811168 , ApJL, 514, L65-68
61. Bias is Complicated
    M Tegmark & B Bromley 2000, Physica Scripta, T85, L59-62
62. Time evolution of galaxy formation and bias in cosmological simulations
    M Blanton, R Cen, J P Ostriker, M A Strauss, M Tegmark 2000, astro-ph/9903165, ApJ, 531, 1-16
63. Is the cosmic microwave background really non-Gaussian?
    B Bromley & M Tegmark 1999, astro-ph/9904254, ApJL, 524, L79-82
64. Cross-correlation of Tenerife data with Galactic templates - evidence for spinning dust?
    A de Oliveira-Costa, M Tegmark, C M Gutierrez, A W Jones, R D Davies, A N Lasenby, R Rebolo & R A Watson 1999, astro-ph/9904296, ApJL, 527, L9-12
65. Decorrelating the power spectrum of galaxies
    A J S Hamilton & M Tegmark 2000, astro-ph/9905192, MNRAS, 312, 285-294
66. Foregrounds and forecasts for the cosmic microwave background
    M Tegmark, D J Eisenstein, W Hu, A de Oliveira-Costa 2000, astro-ph/9905257, ApJ, 530, 133-165
67. The power spectrum of the CfA/SSRS UZC galaxy redshift survey
    N Padmanabhan, M Tegmark & A J S Hamilton 2001, astro-ph/9911421, ApJ, 520, 52-64
68. A spin modulated telescope to make two dimensional CMB maps
    J Staren, P Meinhold, J Childers, M Lim, A Levy, P Lubin, M Seiffert, T Gaier, N Figueiredo, T Villela, C A Wuensche, M Tegmark, A de Oliveira-Costa 2000, astro-ph/9912212, ApJ, 539, 52
69. Current cosmological constraints from a 10 parameter CMB analysis
    M Tegmark & M Zaldarriaga 2000, astro-ph/0002091, ApJ, 541, 535-541
70. Large-Scale Sunyaev-Zel'dovich Effect: Measuring Statistical Properties with Multifrequency Maps
    A Cooray, W Hu, M Tegmark 2000, astro-ph/0002238, ApJ, 540, 1
71. Galactic contamination in the QMAP experiment
    A de Oliveira-Costa, M Tegmark, M J Devlin, L M Haffner, T Herbig, A D Miller, L A Page, R J Reynolds, S L Tufte 2000, astro-ph/0003090, ApJL, 542, L5-8
72. Linear Redshift Distortions and Power in the PSCz Survey
    A J S Hamilton, M Tegmark, N Padmanabhan 2000, astro-ph/0004334, MNRAS, 317, L23
73. New CMB constraints on the cosmic matter budget: trouble for nucleosynthesis?
    M Tegmark & M Zaldarriaga 2000, Phys. Rev. Lett., 85, 2240
74. The dark side of distortion
    M Tegmark 2000, Nature, 405, 133
75. CMB Observables and their cosmological implications
    W Hu, M Fukugita, M Zaldarriaga & M Tegmark 2001, astro-ph/0006436, ApJ, 549, 669-680
76. Towards a refined cosmic concordance model: joint 11-parameter constraints from CMB and large-scale structure
    M Tegmark, M Zaldarriaga, A J S Hamilton 2001, astro-ph/0008165, Phys. Rev. D, 63, 043007-043020
77. Latest cosmological constraints on the densities of hot and cold dark matter
    M Tegmark, M Zaldarriaga & A J S Hamilton 2001, hep-ph/0008145, in Sources and Detection of Dark Matter/Energy in the Universe, ed. D. B. Cline (Springer, Berlin, 2000)
78. Weighing neutrinos with microwave background and galaxy data
    M Tegmark, M Zaldarriaga & A J S Hamilton 2000, Nucl. Phys. B 91, 387-392, in proceedings of XIX International Conference on Neutrino Physics and Astrophysics, Sudbury, Canada, June 2000
79. The Initial Conditions of Galaxy Formation
    M Tegmark, M Zaldarriaga & A J S Hamilton 2001, in The Physics of Galaxy Formation, ed. M. Umemura & H. Susa (ASP Conf. Ser.)
80. Why is the fraction of four-image radio lens systems so high?
    D Rusin & M Tegmark 2001, astro-ph/0008329, ApJ, 553, 709-721
81. The Real Space Power Spectrum of the PSCz Survey from 0.01 to 300 h/Mpc
    A J S Hamilton & M Tegmark 2002, astro-ph/0008392, MNRAS, 330, 506-530
82. A New Spin on Galactic Dust
    A de Oliveira-Costa, M Tegmark, D P Finkbeiner, C M Gutierrez, L M Haffner, A W Jones, A N Lasenby, R Rebolo, R J Reynolds, S L Tufte & R A Watson 2002, astro-ph/0010527, ApJ, 567, 363-369
83. Comparing and combining the Saskatoon, QMAP and COBE CMB maps
    Y Xu, M Tegmark, A de Oliveira-Costa, M J Devlin, T Herbig, A D Miller, C B Netterfield & L Page 2001, astro-ph/0010552, Phys. Rev. D, 63, 103002-103012
84. Constraints from the Lyman alpha forest power spectrum
    M Zaldarriaga, L Hui & M Tegmark 2001, astro-ph/0011559, ApJ, 557, 519-526
85. How to measure CMB polarization power spectra without losing information
    M Tegmark & A de Oliveira-Costa 2001, astro-ph/0012120, Phys. Rev. D, 64;, 063001-063015
86. Measuring the metric: a parametrized post-Friedmanian approach to the cosmic dark energy problem
    M Tegmark 2002, astro-ph/0101354, Phys. Rev. D, 66, 103508-1-10
87. Gaussianity of degree-scale cosmic microwave background anisotropy observations
    Chan-Gyung Park, Changbom Park, Bharat Ratra & Max Tegmark 2001, astro-ph/0102406, ApJ, 556, 582-589
88. The CMB power spectrum at l=30-200 from QMASK
    Yongzhong Xu, Max Tegmark, Angelica de Oliveira-Costa 2002, astro-ph/0104419, Phys. Rev. D, 65, 083002-1-6
89. Is cosmology consistent?
    Xiaomin Wang, Max Tegmark, Matias Zaldarriaga 2002, astro-ph/0105091, Phys. Rev. D, 65, 123001-1-14
90. Galaxy clustering in early SDSS redshift data
    Idit Zehavi, Michael Blanton, Joshua Frieman, David Weinberg, Houjun Mo, Michael Strauss + 60 alphabetized authors (I'm the 53rd...:-) 2002, astro-ph/0102476, ApJ, 571, 172
91. A limit on the large angular scale polarization of the cosmic microwave background
    Brian Keating, Chris O'Dell, Angelica de Oliveira-Costa, Slade Klawikowski, Nate Stebor, Lucio Piccirillo, Max Tegmark & Peter Timbie 2001, astro-ph/0107013, ApJL, 560, L1-4
92. Analysis of systematic effects and statistical uncertainties in angular clustering of galaxies from early SDSS data
    Ryan Scranton, David Johnston, Scott Dodelson, Joshua Frieman et al (I'm 21 out of 47 :-) 2002, astro-ph/0107416, ApJ, 579, 48
93. The angular correlation function of galaxies from early SDSS data
    Andrew Connolly, Ryan Scranton, David Johnston et al (I'm 21 out of 49) 2002, astro-ph/0107417, ApJ, 579, 42
94. The angular power spectrum of galaxies from early SDSS data
    Max Tegmark, Scott Dodelson, Daniel Eisenstein, Vijay Narayanan, Roman Scoccimarro, Ryan Scranton, Michael Strauss et al (41 others) 2002, astro-ph/0107418, ApJ, 571, 191
95. KL estimation of the power spectrum parameters from the angular distribution of galaxies in early SDSS data
    Alexander Szalay, Bhuvnesh Jain, Takahiko Matsubara, Ryan Scranton, Michael S. Vogeley, et al (I'm 26 out of 49) 2003, astro-ph/0107419, ApJ, 591, 1
96. The 3D power spectrum from angular clustering of galaxies in early SDSS data
    Scott Dodelson, Vijay K. Narayanan, Max Tegmark, Ryan Scranton et al (42 others) 2002, astro-ph/0107421, ApJ, 572, 140
97. Gaussianity of the QMASK Map (Morphological Measures of non-Gaussianity in CMB Maps)
    Sergei Shandarin, Hume Feldman, Yongzhong Xu & Max Tegmark 2002, astro-ph/0107136, ApJS, 141, 1-11
98. The power spectrum of galaxies in the 2dF 100k redshift survey
    Max Tegmark, Andrew Hamilton & Yongzhong Xu 2002, astro-ph/0111575, MNRAS, 335, 887-908
99. Cosmic censorship
    M Tegmark 2002, Nature, 415, 374
100. Measuring Spacetime: from the Big Bang to Black Holes
     M Tegmark 2002, Science, 296, 1427-1433
101. First attempt at measuring the CMB cross-polarization
     Angelica de Oliveira-Costa, Max Tegmark, Matias Zaldarriaga, Denis Barkats, Josh O Gundersen, Matt M Hedman, Suzanne T Staggs, Bruce Winstein 2003, astro-ph/0204021, Phys. Rev. D, 67, 023003
102. Two-Dimensional Topology of the Sloan Digital Sky Survey
     Fiona Hoyle, Michael S. Vogeley, J. Richard Gott III, Michael Blanton, Max Tegmark, David H. Weinberg, J. Brinkmann, N. Bahcall 2002, astro-ph/0206146, ApJ, 580, 663-671
103. Separating the Early Universe from the Late Universe: cosmological parameter estimation beyond the black box
     M Tegmark & M Zaldarriaga 2002, astro-ph/0207047, Phys. Rev. D, 66, 103508-1-18
104. E/B decomposition of finite pixelized CMB maps
     Emory Bunn, Matias Zaldarriaga, Max Tegmark & Angelica de Oliveira-Costa 2003, astro-ph/0207338, PRD, 67, 023501
105. The Galaxy Luminosity Function and Luminosity Density at Redshift z=0.1
     Michael R. Blanton, David W. Hogg, J. Brinkmann, Andrew J. Connolly, Istvan Csabai, Neta A. Bahcall, Masataka Fukugita, Jon Loveday, Avery Meiksin, Jeffrey A. Munn, R. C. Nichol, Sadanori Okamura, Thomas Quinn, Donald P. Schneider, Kazuhiro Shimasaku, Michael A. Strauss, Max Tegmark, Michael S. Vogeley & David H. Weinberg 2003, astro-ph/0210215, ApJ, 592, 819
106. The end of unified dark matter?
     Havard Sandvik, Max Tegmark, Matias Zaldarriaga & Ioav Waga 2004, astro-ph/0212114, PRD, 69, 123524
107. The last stand before WMAP: cosmological parameters from lensing, CMB and galaxy clustering
     Xiaomin Wang, Max Tegmark, Bhuvnesh Jain & Matias Zaldarriaga 2003, astro-ph/0212417, PRD, 68, 123001-1-12
108. The Large-Scale Polarization of the Microwave Background and Foreground
     Angelica de Oliveira-Costa, Max Tegmark, Christopher O'Dell, Brian Keating, Peter Timbie, George Efstathiou & George Smoot 2003, astro-ph/0212419, PRD, 68, 083003-1-11
109. CMB Polarization at Large Angular Scales: Data Analysis of the POLAR Experiment
     Christopher W. O'Dell, Brian G. Keating, Angelica de Oliveira-Costa, Max Tegmark & Peter T. Timbie 2003, astro-ph/0212419, PRD, 68, 42002
110. Beyond Cosmological Parameters, M Tegmark 2003, in The Emergence of Cosmic Structure, proc. 13th Annual Astrophysics Conference in Maryland, S. S. Holt & C. Reynolds eds., AIP
111. Cosmology from Large Scale Structure, Andrew Hamilton, Nick Gnedin, Max Tegmark, Yongzhong Xu 2003, astro-ph/0212552, in Particle Physics, H.-V. Klapdor-Kleingrothaus \& R. Viollier eds., Springer
112. On Departures From a Power Law in the Galaxy Correlation Function, Idit Zehavi, David H. Weinberg, Zheng Zheng, Andreas A. Berlind, Joshua A. Frieman, Roman Scoccimarro, Ravi K. Sheth, Michael R. Blanton, Max Tegmark, Houjun J. Mo, et al. 2004, astro-ph/0301280, ApJ, 608, 16
113. A high resolution foreground cleaned CMB map from WMAP
     Max Tegmark, Angelica de Oliveira-Costa & Andrew Hamilton 2003, astro-ph/0302496, PRD, 68, 123523
114. Anthropic predictions for neutrino masses
     Max Tegmark & Alexander Vilenkin 2005, astro-ph/0304536, PRD, 71, 103523
115. The First Data Release of the Sloan Digital Sky Survey, Kev Abazajian et al 2003 (I'm out of 162nd out of 189 alphabetized authors :), astro-ph/0305492, Astron. J., 126, 2081
116. Angular Clustering with Photometric Redshifts in the Sloan Digital Sky Survey: Bimodality in the Clustering Properties of Galaxies, Tamas Budavari, Andrew J. Connolly, Alexander S. Szalay, Istvan Szapudi, Istvan Csabai, Ryan Scranton, Neta A. Bahcall, Jon Brinkmann, Daniel J. Eisenstein, Joshua A. Frieman, Masataka Fukugita, James E. Gunn, David Johnston, Stephen Kent, Jon N. Loveday, Robert H. Lupton, Max Tegmark, Aniruddha R. Thakar, Brian Yanny, Donald G. York, Idit Zehavi 2003, astro-ph/0305603, ApJ, 595, 59
117. The Large-Scale Polarization of the Microwave Foreground, Angelica de Oliveira-Costa, Max Tegmark, Christopher O'Dell, Brian Keating, Peter Timbie, George Efstathiou \& George Smoot 2003, astro-ph/0305590, in proceedings of "The Cosmic Microwave Background and its Polarization", New Astronomy Reviews (eds. S. Hanany & K. A. Olive)
118. Measuring CMB Polarization with BOOMERANG, T. Montroy, P.A.R. Ade, A. Balbi, J.J. Bock, J.R. Bond, J. Borrill, A. Boscaleri, P. Cabella, C.R. Contaldi, B.P. Crill, P. de Bernardis, G. De Gasperis, A. de Oliveira-Costa, G. De Troia, G. di Stefano, K. Ganga, E. Hivon, V.V. Hristov, A. Iacoangeli, A.H. Jaffe, T.S. Kisner, W.C. Jones, A.E. Lange, S. Masi, P.D. Mauskopf, C. Mactavish, A. Melchiorri, F. Nati, P. Natoli, C.B. Netterfield, E. Pascale, F. Piacentini, D. Pogosyan, G. Polenta, S. Prunet, S. Ricciardi, G. Romeo, J.E. Ruhl, E. Torbet, M. Tegmark, N. Vittorio 2003, astro-ph/0305593, in proceedings of "The Cosmic Microwave Background and its Polarization", New Astronomy Reviews (eds. S. Hanany & K. A. Olive)
119. A scheme to deal accurately and efficiently with complex angular masks in galaxy surveys, Andrew J. S. Hamilton & Max Tegmark 2004, astro-ph/0306324, MNRAS, 349, 115
120. The Three-Dimensional Power Spectrum of Galaxies from the Sloan Digital Sky Survey, Max Tegmark, Michael Blanton, Michael A. Strauss, Fiona S. Hoyle, David Schlegel, Roman Scoccimarro, Michael S. Vogeley, David H. Weinberg, Idit Zehavi, Andreas Berlind, Tamas Budavari, Andrew Connolly, Daniel J. Eisenstein, Douglas Finkbeiner, Joshua A. Frieman, Andrew J. S. Hamilton, James E. Gunn, Lam Hui, Bhuvnesh Jain, David Johnston, Stephen Kent, Huan Lin, Reiko Nakajima, Robert C. Nichol, Adrian Pope, Ryan Scranton, Uros Seljak, Ravi K. Sheth, Albert Stebbins, Alexander S. Szalay, Istvan Szapudi, Licia Verde, Yongzhong Xu et al (64 authors in total) 2004, astro-ph/0310725, ApJ, 606, 702-740
121. The significance of the largest scale CMB fluctuations in WMAP, Angelica de Oliveira-Costa, Max Tegmark, Matias Zaldarriaga & Andrew Hamilton 2004, astro-ph/0307282, PRD, 69, 063516
122. Physical evidence for dark energy, R. Scranton, A. J. Connolly, R. C. Nichol, A. Stebbins, I. Szapudi, D. J. Eisenstein, N. Afshordi, T. Budavari, I. Csabai, J. A. Frieman, J. E. Gunn, D. Johnson, Y. Loh, R. H. Lupton, C. J. Miller, E. S. Sheldon, R. S. Sheth, A. S. Szalay, M. Tegmark, Y. Xu, et al 2003, astro-ph/0307335
123. A Map of the Universe, J. Richard Gott III, Mario Juric, David Schlegel, Fiona Hoyle, Michael Vogeley, Max Tegmark, Neta Bahcall, Jon Brinkmann 2005, astro-ph/0310571, ApJ, 624, 463
124. Cosmological parameters from SDSS and WMAP, Max Tegmark, Michael Strauss, Michael R. Blanton, Kev Abazajian, Scott Dodelson, Havard Sandvik, Xiaomin Wang, David H. Weinberg, Idit Zehavi, Neta A. Bahcall, Fiona Hoyle, David Schlegel, Roman Scoccimarro, Michael S. Vogeley, Andreas Berlind, Tamas Budavari, Andrew Connolly Daniel J. Eisenstein, Douglas Finkbeiner, Joshua A. Frieman, James E. Gunn, Lam Hui, Bhuvnesh Jain, David Johnston, Stephen Kent, Huan Lin, Reiko Nakajima, Robert C. Nichol, Jeremiah P. Ostriker, Adrian Pope, Ryan Scranton, Uros Seljak, Ravi K. Sheth, Albert Stebbins, Alexander S. Szalay, Istvan Szapudi, Yongzhong Xu, James Annis, J. Brinkmann, Scott Burles, Francisco J. Castander, Istvan Csabai, Jon Loveday, Mamoru Doi, Masataka Fukugita, Greg Hennessy, David W. Hogg, Zeljko Ivezic, Gillian R. Knapp, Don Q. Lamb, Brian C. Lee, Robert H. Lupton, Timothy A. McKay, Peter Kunszt, Jeffrey A. Munn, Liam O'Connell, John Peoples, Jeffrey R. Pier, Michael Richmond, Constance Rockosi, Donald P. Schneider, Christopher Stoughton, Douglas L. Tucker, Daniel E. Vanden Berk, Brian Yanny and Donald G. York 2004, astro-ph/0310571, PRD, 69, 103501
125. Maps of the millimetre sky from the BOOMERanG experiment, P. de Bernardis et al 2003, astro-ph/0311396
126. CMBfit: Rapid WMAP likelihood calculations with normal parameters, Havard Sandvik, Max Tegmark, Xiaomin Wang & Matias Zaldarriaga 2004, astro-ph/0311544, PRD, 69, 063005
127. The Quest for Microwave Foreground X, Angelica de Oliveira-Costa, Max Tegmark, R.D. Davies, Carlos M. Gutierrez, A.N. Lasenby, R. Rebolo & R.A. Watson 2004, astro-ph/0312039, ApJL, 606, L89
128. Cosmological Parameters from Eigenmode Analysis of Sloan Digital Sky Survey Galaxy Redshifts, A. Pope et al 2004, astro-ph/0401249, ApJ, 607, 655-660
129. New dark energy constraints from supernovae, microwave background and galaxy clustering, Yun Wang & Max Tegmark 2004, astro-ph/0403292, Phys. Rev. Lett., 92, 241302
130. The Second Data Release of the Sloan Digital Sky Survey, Kev Abazajian et al 2004 (144 authors :) 2004, astro-ph/0403325, Astron. J., 128, 502-12
131. The Sloan Digital Sky Survey Commissioning Data: Orion, Douglas Finkbeiner et al 2004, Astron. J., 128, 2577
132. Anthropic predictions for vacuum energy and neutrino masses, Levon Pogosian, Alexander Vilenkin & Max Tegmark 2004, astro-ph/0404497, JCAP, 2004-7, 5
133. How accurately can suborbital experiments measure the CMB?, Angelica de Oliveira-Costa, Max Tegmark, Mark Devlin, Lyman Page, Amber Miller, Barth Netterfield, Yongzhong Xu 2005, astro-ph/0406375, PRD, 71, 043004
134. SDSS galaxy bias from halo mass-bias relation and its cosmological implications, U Seljak, A Makarov, R Mandelbaum, C Hirata, N Padmanabhan, P McDonald, M Blanton, M Tegmark, N Bahcall & J Brinkmann 2005, astro-ph/0406594, PRD, 71, 043511
135. Cosmological parameter analysis including SDSS Ly-alpha forest and galaxy bias: constraints on the primordial spectrum of fluctuations, neutrino mass, and dark energy, U Seljak, A Makarov, P McDonald, S Anderson, N Bahcall, J Brinkmann, S Burles, R Cen, M Doi, J Gunn, Z Ivezic, S Kent, R Lupton, J Munn, R Nichol, J Ostriker, D Schlegel, M Tegmark, D Van den Berk, D Weinberg & D York 2005, astro-ph/0407372, PRD, 71, 103515
136. Cosmology and the Halo Occupation Distribution from Small-Scale Galaxy Clustering in the Sloan Digital Sky Survey, Kevork Abazajian, Zheng Zheng, Idit Zehavi, David H. Weinberg, Joshua A. Frieman, Andreas A. Berlind, Michael R. Blanton, Neta A. Bahcall, J. Brinkmann, Donald P. Schneider & Max Tegmark 2005, astro-ph/0408003, ApJ, 625, 613
137. Non-parametric inversion of strong lensing systems, J M Diego, P Protopapas, H B Sandvik & M Tegmark 2005, astro-ph/0408418, MNRAS, 360, 477
138. The Luminosity and Color Dependence of the Galaxy Correlation Function, I Zehavi, Z Zheng, DH Weinberg, JA Frieman, AA Berlind, MR Blanton, R Scoccimarro, RK Sheth, MA Strauss, I Kayo, Y Suto, M Fukugita, O Nakamura, NA Bahcall, J Brinkmann, JE Gunn, GS Hennessy, Z Ivezic, GR Knapp, J Loveday, A Meiksin, DJ Schlegel, DP Schneider, I Szapudi, M Tegmark, MS Vogeley & DG York 2005, astro-ph/0408569, ApJ, 630, 1-27
139. Multiple universes, cosmic coincidences, and other dark matters, Anthony Aguirre & Max Tegmark 2005, hep-th/0409072, JCAP, 2005-1, 3
140. NYU-VAGC: a galaxy catalog based on new public surveys, Michael R. Blanton, David J. Schlegel, Michael A. Strauss, J. Brinkmann, Douglas Finkbeiner, Masataka Fukugita, James E. Gunn, David W. Hogg, Zeljko Ivezic, G. R. Knapp, Robert H. Lupton, Jeffrey A. Munn, Donald P. Schneider, Max Tegmark \& Idit Zehavi 2005, astro-ph/0410166, Astron. J, 129, 2562-2578
141. The Third Data Release of the Sloan Digital Sky Survey, K. Abazajian et al. (SDSS collaboration; I'm one of 154 alphabetized authors) 2005, astro-ph/0410239, Astron. J, 129, 1755
142. What does inflation really predict?, Max Tegmark 2005, astro-ph/0410281, JCAP, 2005-4, 1
143. The Intermediate-Scale Clustering of Luminous Red Galaxies, Idit Zehavi, Daniel J. Eisenstein, Robert C. Nichol, Michael R. Blanton, David W. Hogg, Jon Brinkmann, Jon Loveday, Avery Meiksin, Donald P. Schneider, Max Tegmark 2005, astro-ph/0411557, ApJ, 621, 22-31
144. Non-parametric mass reconstruction of A1689 from strong lensing data with SLAP, J. M. Diego, H. B. Sandvik, P. Protopapas, M. Tegmark, N. Benitez & T. Broadhurst 2005, astro-ph/0412191, MNRAS, 362, 1247-1258
145. Twenty-one Centimeter Tomography with Foregrounds, Xiaomin Wang, Max Tegmark, Mario Santos & Lloyd Knox 2006, astro-ph/0501081, ApJ, 650, 529
146. Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies, D. J. Eisenstein, I. Zehavi, D. W. Hogg, R. Scoccimarro, M. R. Blanton, R. C. Nichol, R. Scranton, H. Seo, M. Tegmark, Z. Zheng, S. Anderson, J. Annis, N. Bahcall, J. Brinkmann, S. Burles, F. J. Castander, A. Connolly, I. Csabai, M. Doi, M. Fukugita, J. A. Frieman, K. Glazebrook, J. E. Gunn, J. S. Hendry, G. Hennessy, Z. Ivezic, S. Kent, G. R. Knapp, H. Lin, Y. Loh, R. H. Lupton, B. Margon, T. McKay, A. Meiksin, J. A. Munn, A. Pope, M. Richmond, D. Schlegel, D. Schneider, K. Shimasaku, C. Stoughton, M. Strauss, M. SubbaRao, A. S. Szalay, I. Szapudi, D. Tucker, B. Yanny \& D. York 2005, astro-ph/0501171, ApJ, 633, 560-574
147. Uncorrelated Measurements of the Cosmic Expansion History and Dark Energy from Supernovae, Yun Wang & Max Tegmark 2005, astro-ph/0501351, PRD, 71, 103513
148. Cosmological neutrino bounds for non-cosmologists, Max Tegmark 2005, hep-ph/0503257, in "Neutrino Physics", Proceedings of Nobel Symposium 129, eds., L Bergstrom, O. Botner, P. Carlson, P. O. Hulth, and T. Ohlsson
149. Joint Efficient Dark-energy Investigation (JEDI): a Candidate Implementation of the NASA-DOE Joint Dark Energy Mission (JDEM),Wang, Y. et al (I'm one of 12 alphabetized authors), astro-ph/0507043
150. How did it all begin?, Max Tegmark, for 2005 Young Scholars Competition in honor of Charles Townes, astro-ph/0508429
151. Instrument, Method, Brightness and Polarization Maps from the 2003 flight of BOOMERanG, Masi, S. et al (I'm one of 44 alphabetized authors), astro-ph/0507509, AA, 458, 687-716
152. A Measurement of the Angular Power Spectrum of the CMB Temperature Anisotropy from the 2003 Flight of Boomerang, Jones, W.C., et al (I'm one of 37 alphabetized authors) 2006, astro-ph/0507494, ApJ, 647, 823-832
153. A measurement of the polarization-temperature angular cross power spectrum of the Cosmic Microwave Background from the 2003 flight of BOOMERANG, Piacentini, F., et al (I'm one of 37 alphabetized authors) 2006, astro-ph/0507507, ApJ, 647, 833-839
154. A Measurement of the CMB EE Spectrum from the 2003 Flight of BOOMERANG, Montroy, T.E., et al (I'm one of 37 alphabetized authors) 2006, astro-ph/0507514, ApJ, 647, 813-822
155. Cosmological Parameters from the 2003 flight of BOOMERANG, MacTavish, C.J., et al (I'm one of 38 alphabetized authors) 2006, astro-ph/0507503, ApJ, 647, 799-812
156. The Fourth Data Release of the Sloan Digitial Sky Survey, Adelman-McCarthy, JK, et al 2006, astro-ph/0507711, ApJS, 162, 38-48
157. Limits on non-Gaussianities from WMAP data,P Creminelli, A Nicholis, L Senatore, M Tegmark & M Zaldarriaga 2006, astro-ph/0509029, JCAP, 0605, 004
158. Combined reconstruction of weak and strong lensing data with WSLAP, J.M. Diego, M. Tegmark, P. Protopapas, H.B. Sandvik, astro-ph/0509103, MNRAS, 375, 958-970
159. How Unlikely is a Doomsday Catastrophe?, M Tegmark & N Bostrom 2005, astro-ph/0512204, Nature, 438, 754
160. On Math, Matter and Mind, P Hut, M Alford, M Tegmark 2006, physics/0510188, Found. Physics, 36, 765-794
161. Dimensionless constants, cosmology and other dark matters, M Tegmark, A Aguirre, M J Rees, F Wilczek 2006, astro-ph/0511774, PRD, 73, 023505
162. CMB multipole measurements in the presence of foregrounds, A de Oliveira-Costa, M Tegmark 2006, astro-ph/0603369, PRD, 74, 023005
163. Task Force on Cosmic Microwave Background Research, J Bock et al (I'm one of 14 alphabetized authors), 2006, astro-ph/0604101. Final Report of the DoE/NASA/NSF Interagency Task Force on CMB Research.
164. The Clustering of Luminous Red Galaxies in the Sloan Digital Sky Survey Imaging Data, N Padmanabhan et al (I'm one of 20 alphabetized authors), 2006, astro-ph/0605302, MNRAS, 378, 852-872
165. Constraining Torsion with Gravity Probe B, Y Mao, M Tegmark, A Guth & S Cabi, 2006, gr-qc/0608121, PRD, 76, 104029
166. Cosmological Constraints from the SDSS Luminous Red Galaxies, M Tegmark et al 2006, astro-ph/0608632, PRD, 74, 123507
167. The shape of the SDSS DR5 galaxy power spectrum, W J Percival et al (I'm one of 17 alphabetized authors), 2007, astro-ph/0608636, ApJ, 657, 645-663
168. Limits on f_NL parameters from WMAP 3yr data, P Creminell, L Senatore, M Zaldarriaga, M Tegmark, 2006, astro-ph/0610600, JCAP, 03, 005
169. Constraining f(R) Gravity as a Scalar Tensor Theory, T Faulkner, M Tegmark, E Bunn, Y Mao, 2007, astro-ph/0612569, PRD, 76, 063505
170. SDSS Galaxy Clustering: Luminosity & Color Dependence and Stochasticity, Molly E.C. Swanson, Max Tegmark, Michael Blanton, Idit Zehavi, astro-ph/0702584, MNRAS, 385, 1635
171. CMB Polarization with Boomerang 2003, F. Piacentini et al (I'm one of 40 alphabetized authors), 2007, New Astronomy Reviews, 51, pp. 244-249.
172. Searching for non Gaussian signals in the BOOMERanG 2003 CMB maps, G. De Troia et al (I'm one of 41 alphabetized authors), 2007, arxiv:0705.1615 [astro-ph], ApJ, 670, L73-76
173. Searching for non Gaussian signals in the BOOMERanG 2003 CMB maps: Preliminary Results, G. De Troia et al (I'm one of 41 alphabetized authors), 2007, New Astronomy Reviews, 51, 250-255
174. The millimeter sky as seen with BOOMERanG, S. Masi et al (I'm one of 44 alphabetized authors), 20047, New Astronomy Reviews, 51, 236-243
175. Observations of the temperature and polarization anisotropies with BOOMERANG 2003, WC Jones et al (I'm one of 38 alphabetized authors), 2007, New Astronomy Reviews, 50, 945-950
176. The Sixth Data Release of the Sloan Digital Sky Survey, JK Adelman-McCarthy et al (I'm one of 100 alphabetized authors), 2007, arxiv:0707.3413 [astro-ph], ApJS, 172, 634
177. Searching for Inflation in Simple String Theory Models: An Astrophysical Perspective, MP Hertzberg, M. Tegmark, S. Kachru, J. Shelton, and O. Ozcan, 2007, arxiv:0709.0002 [astro-ph], PRD, 76, 103521
178. Inflationary Constraints on Type IIA String Theory, M. P. Hertzberg, S. Kachru, W. Taylor, M Tegmark, arxiv:0711.2512 [hep-th], JHEP, 12, 95
179. Methods for Rapidly Processing Angular Masks of Next-Generation Galaxy Surveys, M. Swanson, M. Tegmark, A. J. S. Hamilton, J. C. Hill, arxiv:0711.4352 [astro-ph], MNRAS, 387, 1391
180. A model of diffuse Galactic Radio Emission from 10 MHz to 100 GHz, A. de Oliveira-Costa, M. Tegmark, B. M. Gaensler, J. Jonas, T. L. Landecker and P. Reich, arxiv:0802.1525 [astro-ph], MNRAS, 388, 247
181. How accurately can 21 cm tomography constrain cosmology?, Y. Mao, M. Tegmark, M. McQuinn, M. Zaldarriaga and O. Zahn, arxiv:0802.1710 [astro-ph], PRD, 78, 023529
182. The Fast Fourier Transform Telescope, M Tegmark & M Zaldarriaga 2008, arxiv:0805.4414 [astro-ph], PRD, 79, 083530
183. Axion cosmology and the energy scale of inflation, M P Hertzberg, M Tegmark & F Wilczek 2008, arxiv:0807.1726 [astro-ph], PRD, 78, 083507
184. Will point sources spoil 21 cm tomography?, A. Liu, M. Tegmark and M. Zaldarriaga 2009, arxiv:0807.3952 [astro-ph], MNRAS, 394, 1575
185. The Seventh Data Release of the Sloan Digital Sky Survey, J. K. Adelman-McCarthy et al (I'm one of about 10² alphabetized authors), arxiv:0812.0649 [astro-ph], ApJS, 182, 543
186. Astrophysics from the Highly-Redshifted 21 cm Line, S Furlanetto et al (I'm one of 29 authors), arxiv:0902.3011 [astro-ph], science white paper submitted to the US Astro2010 Decadal Survey "Galaxies across Cosmic Time" Science Frontier Panel
187. Cosmology from the Highly-Redshifted 21 cm Line, S Furlanetto et al (I'm one of 29 authors), arxiv:0902.3259 [astro-ph], science white paper submitted to the US Astro2010 Decadal Survey "Cosmology and Fundamental Physics" Science Frontier Panel
188. Non-Gaussianity as a Probe of the Physics of the Primordial Universe and the Astrophysics of the Low Redshift Universe, E Komatsu et al (I'm one of 61 authors), arxiv:0902.4759 [astro-ph], science white paper submitted to the US Astro2010 Decadal Survey "Cosmology and Fundamental Physics" Science Frontier Panel
189. Observing the Evolution of the Universe, J Aguirre et al (I'm one of 177 alphabetized authors), arxiv:0903.0902 [astro-ph], science white paper submitted to the US Astro2010 Decadal Survey "Cosmology and Fundamental Physics" Science Frontier Panel
190. Likely values of the Higgs vacuum expectation value, '', J F Donoghue, K Dutta, A Ross & M Tegmark 2009, arxiv:0903.1024 [astro-ph], PRD, 81, 073003
191. An Improved Method for 21cm Foreground Removal, A Liu, M Tegmark, J Bowman, J Hewitt & M Zaldarriaga 2009, arxiv:0903.4890 [astro-ph], MNRAS, 398, 401
192. The Second Law and Cosmology, M Tegmark 2009, arxiv:0904.3931 [pop-ph], in Meeting the Entropy Challenge, eds. G P Beretta, A F Ghoneim & G N Hatsopoulos, AIP, New York
193. Subdegree Sunyaev-Zel'dovich Signal from Multifrequency BOOMERanG observations, M Veneziani et al 2009 (I'm one of 38 authors), arxiv:0904.4313 [astro-ph], ApJL, 702, L61
194. BOOMERanG Constraints on Primordial Non-Gaussianity from Analytical Minkowski Functionals, P Natoli et al 2009 (I'm one of 35 authors), arxiv:0905.4301 [astro-ph], MNRAS, 408, 1658
195. Cosmological Constraints from the Clustering of the Sloan Digital Sky Survey DR7 Luminous Red Galaxies, B Reid et al 2009 (I'm one of 28 authors), arxiv:0907.1659 [astro-ph], MNRAS, 404, 60
196. Baryon Acoustic Oscillations in the Sloan Digital Sky Survey Data Release 7 Galaxy Sample, W J Percival et al 2009 (I'm one of 26 authors), arxiv:0907.1660 [astro-ph], MNRAS, 401, 2148
197. Omniscopes: Large Area Telescope Arrays with only N log N Computational Cost, M Tegmark & M Zaldarriaga 2009, arxiv:0909.0001 [astro-ph], PRD, 82, 103501
198. Solving the Corner-Turning Problem for Large Interferometers, A Lutomirski, M Tegmark, N Sanchez, L Stein & M Zaldarriaga 2011, arxiv:0910.1351 [astro-ph], MNRAS, 410, 2075
199. Precision Calibration of Radio Interferometers Using Redundant Baselines, A Liu, M Tegmark, S Morrison, A Lutomirski & M Zaldarriaga 2009, arxiv:1001.5268 [astro-ph], MNRAS, 408, 1029
200. Galaxy Clustering in the Completed SDSS Redshift Survey: The Dependence on Color and Luminosity, Idit Zehavi et al (I'm one of 18 authors) 2011, arxiv:1005.2413 [astro-ph], ApJ, 736, 59
201. Testing Two-Field Inflation, Courtney Peterson & Max Tegmark 2011, arxiv:1005.4056 [astro-ph], PRD, 83, 023522
202. Born in an Infinite Universe: a Cosmological Interpretation of Quantum Mechanics, Anthony Aguirre & Max Tegmark 2011, arxiv:1008.1066 [quant-ph], PRD, 84, 105002
203. Non-Gaussianity in Two-Field Inflation, Courtney Peterson & Max Tegmark 2011, arxiv:1011.6675 [astro-ph], PRD, 84, 023520
204. A method for 21 cm power spectrum estimation in the presence of foregrounds, Adrian Liu & Max Tegmark 2011, arxiv:1103.0281 [astro-ph], PRD, 83, 103006
205. How well can we measure and understand foregrounds with 21cm experiments?, Adrian Liu & Max Tegmark 2012, arxiv:1106.0007 [astro-ph], MNRAS, 419, 3491
206. Testing Multi-Field Inflation: A Geometric Approach, Courtney Peterson & Max Tegmark 2011, arxiv:1111.0927 [astro-ph], submitted to PRD
207. A Fast Method for Power Spectrum and Foreground Analysis for 21 cm Cosmology, Josh Dillon, Adrian Liu \& Max Tegmark 2012, arxiv:1211.2232 [astro-ph], submitted to PRD
208. Global 21cm Signal Experiments: A Designer's Guide, Adrian Liu, Jonathan Pritchard, Max Tegmark & Abraham Loeb 2012, arxiv:1211.3743 [astro-ph], PRD, in press
209. How unitary cosmology generalizes thermodynamics and solves the inflationary entropy problem, Max Tegmark 2012, PRD, 85, 123517

Non-cosmology publications

210. Apparent wave-function collapse caused by scattering M Tegmark 1993, Found. Phys. Lett., 6, 571-590
211. Steady states of harmonic oscillator chains and shortcomings of harmonic heat baths
     M Tegmark & L Yeh 1994, Physica A, 202, 342-362
212. An elementary proof that the biharmonic Green function of an eccentric ellipse changes sign
     H Shapiro & M Tegmark 1994, Soc. Ind. App. Math. Rev., 36, 99-101
213. Decoherence produces coherent states: an explicit proof for harmonic chains
     M Tegmark & H Shapiro 1994, Phys. Rev. E, 50, 2538-2547
214. Does the universe in fact contain almost no information?
     M Tegmark 1996, Found. Phys. Lett., 9, 25-42
215. The economics of Lake Kariba
     J Oldhoff & M Tegmark 1989, Swedish International Development Agency
216. Particle-like solutions of the SU(2) Einstein-Yang-Mills equations
     M Tegmark 1990, B. Sc. thesis, Royal Inst. of Technology, Stockholm, Sweden
217. Measuring quantum states:
     an experimental setup for measuring the spatial density matrix
     M Tegmark 1996, Phys. Rev. A., 54, 2703-2706
218. Is ``the theory of everything'' merely the ultimate ensemble theory?
     M Tegmark 1998, Annals of Physics,  270, 1-51
219. On the dimensionality of spacetime
     M Tegmark 1997, Classical and Quantum Gravity, 14, L69-L75
220. The interpretation of quantum mechanics: many worlds or many words?
     M Tegmark 1998, Fortschr. Phys. 46, 855-862
221. The importance of quantum decoherence in brain processes
     M Tegmark 2000, quant-ph/9907009, Phys. Rev. E 61, 4194-4206
222. Why the brain is probably not a quantum computer
     M Tegmark 2000, Information Sciences 128, 155-179
223. 100 Years of quantum mysteries
     M Tegmark & John Archibald Wheeler 2001, quant-ph/0101063, Scientific American Feb. 2001, 68-75
224. Parallel Universes
     M Tegmark 2003, astro-ph/0302131, Scientific American May 2003, 40-51 (cover story)
225. The Mathematical Universe, M Tegmark 2007, 0704.0646/gr-qc, Founds. Phys. November 2007, 116
226. Many lives in many worlds, M Tegmark 2007, Nature 448, 23
227. Shut up and calculate, M Tegmark 2007, New Scientist September 15, (cover story)
228. Relativity Revisited, F. Lopis & M. Tegmark 2008, arxiv:0804.0016 [astro-ph] (April Fool's joke)
229. The Multiverse Hierarchy, M Tegmark 2009, arxiv:0905.1283 [pop-ph], in Universe or Multiverse?, B Carr ed., Cambridge University Press
230. Many Worlds in Context, M Tegmark 2009, arxiv:0905.2182 [quant-ph], in Many Worlds? Everett, Quantum Theory and Reality, S Saunders, J Barrett, A Kent & D Wallace (eds)

Edited Book

Microwave Foregrounds
Eds. A de Oliveira-Costa & M Tegmark 1999 (ASP, San Francisco), 377 page review volume

OVERVIEW OF MY PAPERS (full list above)
Summary
After graduate work on the role of atomic and molecular chemistry in cosmic reionization, I have mainly focused my research on issues related to constraining cosmological models. A suite of papers developed methods for analyzing cosmological data sets using information theory and applied them to various CMB experiments and galaxy redshift surveys, often in collaboration with the experimentalists who had taken the data. Another series of papers tackled various ``dirty laundry'' issues such as microwave foregrounds and mass-to-light bias. Other papers, most recently these, develop and apply techniques for clarifying the big picture in cosmology: comparing and combining diverse cosmological probes, cross-checking for consistency and constraining cosmological models and their free parameters. My main current research interest is cosmology theory and phenomenology. I'm particularly enthusiastic about the prospects of combining current and upcoming data on CMB, LSS, galaxy clusters, lensing, LyA forest clustering, SN 1, etc. to raise the ambition level beyond the current cosmological parameter game, testing rather than assuming the underlying physics. This paper and this one contain my battle cry.

The big picture: constraining cosmological models
A series of papers used information theory to estimate how accurately different cosmological observables could constrain cosmological parameters, to aid survey design etc: CMB, LSS, weak lensing, SN Ia and CMB+LSS for the neutrino mass, the Hubble parameter, mystery matter, and in gory detail. Another series used the latest data to constrain cosmological parameters in practice: 1998, 2000 (incl. new fast C_l method), after Boomerang 2000, after 2001 Boom + DASI+Maxima, and with WMAP+SDSS 2003. Are different observations consistent? Here are tests 1994, 2001 and 2003.

CMB analysis & modeling
I also have a strong interest in low-level nuts-and-bolts analysis and interpretation of data, firmly believing that the devil is in the details. Indeed, most of my papers are in this more grueling technical category. Although CMB is exciting and promising, there are some skeletons in the closet. Three real-world issues have worried me a lot: foregrounds, numerical problems and systematic errors. Dozens of my papers have tackled these real-world issues related to doing precision cosmology in practice, not merely in principle. These papers all relate to different parts of this schematic analysis pipeline.   Well-known microwave foregrounds are synchrotron, free-free and dust emission from our own Galaxy as well as extragalactic point sources. One of my most referenced papers discussed how they differed from CMB not only in their frequency dependence, but also in their spatial clustering properties, and how this could be used to remove them more efficiently. I've since generalized this method for real-world foregrounds whose frequency dependence varies across the sky and to the non-Gaussian case of removing point sources. In the latter case, weak gravitational lensing effects also enter. By cross-correlating different maps, I've helped quantify the contamination at in the QMAP, Tenefife, COBE and 19 GHz experiments, detecting synchrotron, dust, free-free and a mystery foreground, all described on Angelica's foreground page. My theoretical work on reionization and the resulting spectral and spatial distortions can also be thought of as a foreground messing up the primordial CMB signal, especially when it is patchy. But one person's noise is somebody else's signal: the kinematic SZ-effect will allow measurements of cluster bulk flows on 100-500 Mpc scales with error bars of the order of 100 km/s, and Planck may produce a useful catalog of 40,000 far infra-red point sources. Everything I knew about foregrounds as of year 2000 is in our 30-page monster paper.

By numerical issues, I mean the challenge of building a data-analysis pipeline that extracts the information from CMB data in practice, in a reasonable amount of CPU time, which is easier said than done given the huge size of upcoming data sets. You'll find my ideas for how do this on my pipeline page - here's a brief summary of what I've done. I'm interested in all steps of the pipeline, from experimental design to pixelization, mapmaking, map merging, foreground removal, power spectrum estimation with incomplete sky coverage and parameter estimation. I think it is useful to think of the entire pipeline in terms of information theory and data compression, as described in more detail here and here. Mapmaking is an important step in the pipeline whereby huge data sets can be reduced to a more manageable size without losing any cosmological information. We used such lossless techniques when making the Saskatoon, HACME, QMAP and QMASK maps, and I'm currently working on other data sets. For maps with less than about 10⁴ pixels, the brute-force approach to parameter estimation that I introduced for the 2 year COBE data and applied to the combined COBE and Tenerife data sets is feasible and gives minimal error bars, which is why it was subsequently adopted by the COBE team in their 4 year data analysis. Linear data compression techniques constitute a powerful tool for getting the same answer orders of magnitudes faster. They are also a great tool for spotting systematic errors, as we showed with the first and second flights of QMAP. For future megapixel maps, however, another data compression step will probably have to be added to make the pipeline computationally feasible: power spectrum estimation. This is complicated by incomplete sky coverage, but I have shown that the angular power spectrum C_l can be measured with minimal error bars with a simple quadratic method. I have applied it to the COBE and QMASK data, and extensions of this method have now been successfully applied to, e.g, the Boomerang and Maxima data sets and to a full-blown simulation of the megapixel MAP data set by Oh, Spergel & Hinshaw. This method works for arbitrary incomplete sky coverage, and good news for experimental design is that it gives window functions narrow enough to avoid blurring out features in the power spectrum as long as the sky patch covered is a few degrees wide in the narrowest direction.

LSS analysis & modeling
  Just like the CMB, galaxy redshift surveys are a potential powerful probe of cosmological parameters, and with a set of skeletons in the closet. Three of them have worried me a lot: bias, numerical problems and extinction. Many of my papers have tackled these real-world issues related to doing precision cosmology in practice, not merely in principle. The problem of bias refers to the fact that that the underlying matter distribution (which we would like to measure) can be different from the galaxy distribution (which we do measure). It has become increasingly clear that bias is (just like CMB foregrounds!) more complicated than some had assumed. The simplest assumption - that the galaxy fluctuations are simply proportional to the density fluctuations - is no longer tenable. This proportionality constant (called b) depends on scale and time. Moreover, at least on small scales, the relation is probably nonlinear stochastic, with a scatter due to gas physics etc - I've helped model this both analytically and with simulations and demonstrated it observationally with the LCRS survey. Good news is that you can still measure cosmological parameters by incorporating all these complications into a single unknown function r(k), the correlation between galaxies and mass, and measure this using redshift distortions, so all is not lost.

Just as for the CMB, there are serious numerical problems associated with analyzing these huge upcoming redhift surveys. Since the observational efforts going into large-scale structure data collection are so large, both for to galaxy surveys and CMB experiments, I feel that it is our duty as theorists to develop fairly optimal tools for the data analysis step, thereby making the most of the data. In this spirit, I've helped develop new techniques for estimating the power spectrum P(k) from galaxy surveys that include the complications of survey geometry, integral constraints and extinction errors and produce uncorrelated error bars. I've helped apply this to the UZC, PSCz (1 + 2) and 2dF redshift surveys and to the SDSS. I'm currently having fun working on several further SDSS projects.

Side interests
I have side interests in early galaxy formation, gamma-ray bursts, quantum decoherence, math problems and crazy stuff, all described above - click on the above links to read about the corresponding papers.